LIGO-IndiaDetecting Einsteinrsquos Elusive Waves

Opening a New Window to the Universe

An Indo-US joint mega-project concept proposal

IndIGO Consortium(Indian Initiative in Gravitational-wave Observations)

Version BRI Jun 10 2011wwwgw-indigoorg

In 1916 Albert Einstein published his famous Theory of General Relativity the theory of gravitation4-dimensional space-time (the normal three dimensions of space plus a fourth dimension of time)

His theory describes how space-time is affected by mass and also how mass affects spacetime Matter tells spacetime how to curve and spacetime tells matter how to move

Space Time as a fabric

Space Time as a fabric

Einsteinrsquos General theory of relativity is the most beautiful amp successful theory of modern physics It has matched all tests of Gravitation remarkably well

What happens when matter is in motion

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

In 1916 Albert Einstein published his famous Theory of General Relativity the theory of gravitation4-dimensional space-time (the normal three dimensions of space plus a fourth dimension of time)

His theory describes how space-time is affected by mass and also how mass affects spacetime Matter tells spacetime how to curve and spacetime tells matter how to move

Space Time as a fabric

Space Time as a fabric

Einsteinrsquos General theory of relativity is the most beautiful amp successful theory of modern physics It has matched all tests of Gravitation remarkably well

What happens when matter is in motion

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Space Time as a fabric

Einsteinrsquos General theory of relativity is the most beautiful amp successful theory of modern physics It has matched all tests of Gravitation remarkably well

What happens when matter is in motion

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Einsteinrsquos General theory of relativity is the most beautiful amp successful theory of modern physics It has matched all tests of Gravitation remarkably well

What happens when matter is in motion

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

What happens when matter is in motion

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Einsteinrsquos theory predicts

Matter in motion fluctuation in the curvature of space-time which propogates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

GW from Binary Neutron stars

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

1 leads to loss of orbital energy

2 period speeds up 14 sec from 1975-94

3 measured to ~50 msec accuracy

4 deviation grows quadratically with time

Binary pulsar emits gravitational waves

Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Won the Nobel prizein 1993

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Detecting GW with Laser Interferometer

Difference in distance of Path A amp B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer

Equal arms Dark fringe

Unequal arm Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain h(change in lengthoriginal length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion

Gravitational waves are very weak

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

GW Astronomy with Intl Network of GW Observatories

LIGO-LLO 4km

LIGO-LHO 2km 4kmGEO 06km VIRGO 3km

TAMA 03km

LIGO-Australia

1 Detection confidence 2 Duty cycle 3 Source direction 4 Polarization info

LIGO-India

LCGT

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

A Century of Waitingbull Almost 100 years since GW were theoretically predicted By Albert

Einstein but still no direct experimental confirmation a la Hertzbull Reason is connected to two fundamental differences between EM andGravitation - The weakness of the gravitational interaction relative to EM (10104857639) -The spin two nature of gravitation compared to the spin one nature of EM that forbids dipole radiation in GRbull Implies low efficiency for conversion of mechanical energy to

gravitational radiation And feeble effects of GW on any potential detector

bull A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Gravitational Waves ExistHigh quality data which is proof that GW exist In 1974 Hulse and Taylor discovered the Binary Pulsar 1913+16 The system has now been monitored for 30 years Orbital period slowly decreasing at just the rate predicted by GR for emission of GWHulse and Taylor received Nobel Prize for this (1993)

ADD FIGURES

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Laser Interferometric Gravitational Wave Detectors

bull Binary Pulsars establish Reality of Grav Radn Validity of GR in Strong Fields Excellent Evidence but Evidence is Indirect

bull Can detectors be built to attempt a Direct detection of these GWbull GW are transverse and tidally distort a system in directionsperpendicular to propagation directionbull Effect measured by the Dimensionless strain h = 2( Delta L) L it producesFor a typical NS binary in Virgo cluster (18 Mpc 56 x 10^20 km)h = 4G c^4 KnonsphD ~ (2 GM Rc^2) (GMDc^2) ~ 15 x 10^-21bull The miniscule strain and associated tiny displacement must bemeasured to detect the GW bull Webers Bar detectors (Narrow band) Todays Laser Interferometric Detectors ( Broad Band)bull As a GW passes the arm lengths of km scale ITF change (10^-18m)tidally causing the interference pattern to change at the photodiodebull Direct detection of GW -First mandate of Laser Interferometric GW detectorsbull Promised and Real Excitement - New Observational Window andTool for Astrophysics Experimental Probe for Basic Physics

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources Improve on Spindown of Crab Vela pulsars Big Bang nucleosynthesis bound on Stochastic GW

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Expected Annual Coalescence RatesIn a 95 condence interval rates uncertain by 3 orders of magnitudeNS-NS (04 - 400) NS-BH (02 - 300) BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary PulsarsStellar birth rateestimates Population Synthesis models Rates quoted below are mean of the distribution

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 002 00006 00009

Enhanced LIGO(2X Sensitivity)(2009-2010)

01 004 007

Advanced LIGO(10X sensitivity)(2014 - hellip)

40 10 200

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Laser Interferometer GW Observatory

4 km 12m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO U

K)

Optics amp controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Schematic Optical Design of Advanced LIGO detectors

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

If retained get better res picture

Era of Advanced LIGO detectors 2015

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Courtesy B Schutz GWIC Roadmap Document 2010

Gravitational wave Astronomy Synergy with other major Astronomy projects

bull SKA Radio Pulsars timing bull X-ray satellite (AstroSAT)bull Gamma ray observatorybull Thirty meter telescope gamma ray follow-uphellipbull bull

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

INDIGO the goalsbull Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)ndash Advanced LIGO hardware for 1 detector to be shipped to Indiandash India provides suitable site and infrastructure to house the GW observatoryndash Site two 4km armlength high vacuum tubes in L configndash Indian cost ~Rs 1000Cr Earlier plan Partnership in LIGO-Australia (a diminishing possibility)

ndash Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site near Perth NSF approvalndash Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a yearndash Indian partnership at 15 of Australian cost with full data rights

bull Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

bull Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower ndash 3m prototype detector in TIFR (funded) Unnikrishnanndash Laser expt RRCAT IIT M IIT K | High Vaccum amp controls at RRCAT IPR BARC ISRO hellipndash UG summer internship at Natn amp Intl GW labs amp observatoriesndash Postgrad IndIGO schools specialized courseshellip

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Multi-InstitutionalMulti-disciplinary Consortium

1 CMI Chennai2 Delhi University3 IISER Kolkata4 IISER Trivandrum5 IIT Madras6 IIT Kanpur7 IUCAA8 RRCAT9 TIFR

bull RRIbull IPR Bhattbull Jamia Milia Islamiabull Tezpur Univ

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

The IndIGO Consortium

Data Analysis amp Theory

1 Sanjeev Dhurandhar IUCAA2 Bala Iyer RRI3 Tarun Souradeep IUCAA4 Anand Sengupta Delhi University 5 Archana Pai IISER Thiruvananthapuram6 Sanjit Mitra JPL IUCAA7 K G Arun Chennai Math Inst Chennai8 Rajesh Nayak IISER Kolkata9 A Gopakumar TIFR Mumbai 10 T R Seshadri Delhi University 11 Patrick Dasgupta Delhi University12 Sanjay Jhingan Jamila Milia Islamia Delhi13 L Sriramkumar Phys IIT M14 Bhim P Sarma Tezpur Univ 15 P Ajith Caltech USA16 Sukanta Bose Wash U USA17 B S Sathyaprakash Cardiff University UK18 Soumya Mohanty UTB Brownsville USA19 Badri Krishnan Max Planck AEI Germany

Instrumentation amp Experiment

1 C S Unnikrishnan TIFR Mumbai2 G Rajalakshmi TIFR Mumbai3 PK Gupta RRCAT Indore 4 Sendhil Raja RRCAT Indore5 SK Shukla RRCAT Indore6 Raja Rao ex RRCAT Consultant 7 Anil Prabhakar EE IIT M8 Pradeep Kumar EE IIT K9 Ajai Kumar IPR Bhatt10 SK Bhatt IPR Bhatt 11 Ranjan Gupta IUCAA Pune12 Rijuparna Chakraborty Cote drsquoAzur Grasse13 Rana Adhikari Caltech USA 14 Suresh Doravari Caltech USA 15 Biplab Bhawal (ex LIGO)

IndIGO Council1 Bala Iyer ( Chair) RRI

Bangalore 2 Sanjeev Dhurandhar (Science) IUCAA Pune 3 C S Unnikrishnan (Experiment) TIFR Mumbai4 Tarun Souradeep (Spokesperson) IUCAA Pune

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Committees National Steering CommitteeKailash Rustagi (IIT Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]DD Bhawalkar (Quantalase Indore)[Advisor]PK Kaw (IPR)Ajit Kembhavi (IUCAA) PD Gupta (RRCAT)JV Narlikar (IUCAA)G Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO Caltech USA)David Blair (AIGO UWA Australia)Adalberto Giazotto (Virgo Italy)PD Gupta (Director RRCAT India)James Hough (GEO Glasgow UK)[GWIC Chair]Kazuaki Kuroda (LCGT Japan)Harald Lueck (GEO Germany)Nary Man (Virgo France)Jay Marx (LIGO Director USA)David McClelland (AIGO ANU Australia)Jesper Munch (Chair ACIGA Australia)BS Sathyaprakash (GEO Cardiff Univ UK)Bernard F Schutz (GEO Director AEI Germany)Jean-Yves Vinet (Virgo France)Stan Whitcomb (LIGO Caltech USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR Mumbai) ChairBala R Iyer (RRI Bangalore) CoordinatorSanjeev Dhurandhar (IUCAA Pune) Co-cordinatorTarun Souradeep (IUCAA Pune)Bhal Chandra Joshi (NCRA Pune)P Sreekumar (ISAC Bangalore)P K Gupta (RRCAT Indore)S K Shukla (RRCAT Indore)Sendhil Raja (RRCAT Indore)

INSERT BOX

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India Why is it a good ideafor India

bull Has a 20 year legacy and wide recognition in the Intl GW community with seminal contributions to Source modeling (RRI)amp Data Analysis (IUCAA) High precision measurements (TIFR) Participation in LHC (RRCAT)

bull (Would not make it to the GWIC report otherwise)ndash AIGOLIGOEGO strong interest in fostering Indian communityndash GWIC invitation to IndIGO join as member (July 2011)

bull Provides an exciting challenge at an International forefront of experimental science Can tap and siphon back the extremely good UG students trained in India (Sole cause of `brain drainrsquo)

ndash 1st yr summer intern 2010 MIT for PhDndash Indian experimental scientist Postdoc at LIGO training for Adv LIGO subsystem

bull Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India

ndash Sendhil Raja RRCAT Anil Prabhakar EE IIT Madras Pradeep Kumar EE IITK Photonicsndash Vacuum expertise with RRCAT (SK Shukla AS Raja Rao) IPR (SK Bhatt Ajai Kumar)

bull Jump start direct participation in GW observationsastronomy ndash going beyond analysis methodology amp theoretical prediction --- to full fledged participation in

experiment data acquisition analysis and astronomy results

bull For once may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed Once in a generation opportunity to host an Unique International Experiment here

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India Why is it a good ideahellip for the World

bull Strategic geographical relocation for GW astronomyndash sky coverage gainndash distancendash duty cycle

bull Potentially large science community in futurendash Indian demographics youth dominated ndash need challengesndash excellent UG education system already produces large number of trained

in India find frontline research opportunity at home

bull Large data analysis trained manpower and facilities exist (and being created

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Courtesy B Schutz GWIC Roadmap Document

GWIC Gravitational Wave International Committee

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Indo-AusMeeting Delhi Feb 2011

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

23 July 2011Dear Bala

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membershiphelliphellip

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India the concept hellipbull LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

bull Advanced LIGO interferometer detector funded and ready to be shipped by US

bull Indian contribution in infrastructure site vacuum systemRelated ControlsData centre trained manpower for installation

commissioning and running for 10 years

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

bull New Physics New Astronomy New Astrophysics New Cosmologybull A New Window ushers a new era of explorationbull Testing Einsteins GRbull Black hole phenomenabull Understanding nuclear matter by neutron star EOSbull Neutron star coalescence eventsbull Listening to most energetic events in the universe Supernovae Gamma ray bursts Magnetarsbull New Cosmology Standard SirensDetermine EOS of Dark energybull Multi-messenger AstronomyThe Unexpected

The Science payoffs

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

bull Lasers and optics Purest laser light - Low phase noise excellentbeam quality high single frequency power bull Applications in precision metrology medicine micro-machiningbull Coherent laser radar and strain sensors for earthquake prediction and other precision metrologybull Surface accuracy of mirrors 100 times better than telescope mirrorsUltrahigh reflective coatingsbull Vibration isolation and suspensionApplications for mineralprospectingbull Sqeezing and QM limitsbull Ultra high vacuum system 10^-9 torrbull Largest in this region bull Computation Challenges

f

The Technology Payoffs

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the Opportunity

bull Part of a fundamental scientific discovery direct detection of gravitational radiation

bull Part of ldquohistoricrdquo launch of a new window of Astronomybull LIGO-India Southernmost hence Unique role in the

Intl GW observatory network

bull Full detector at about half the cost is the naiumlve calculation

Adv LIGO detector system is worth 15 years of challenging R ampD ndash price tag

bull Indian Labs amp Industry bull bull

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage Synthesized Network beam(antenna power)

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunity

Strategic Geographical relocation- the science gain

Sky coverage lsquoreachrsquo sensitivity in different directions

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree

Ellipses version as in LIGO-Aus proposal

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunityStrategic Geographical relocation

Polarization info

Sky coverage

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunity

Strategic Geographical relocation

Network HIJLV GMRT BangaloreMean horizon distance 157 163Detection Volume 120 120Volume Filling factor 73 66Triple Detection Rate(80) 862 864Triple Detection Rate(95) 111 111Sky Coverage 100 100Directional Precision 293 300

Figure

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunityLIGO-India Technology gain

bull 180 W pre-stablized NdYAG laser

bull Input condition optics including electro-optic modulators Faraday isolators a suspended mode-cleaner (12-m long mode-defining cavity) and suspended mode-matching telescope optics

bull five BSC chamber seismic isolation systems (two stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull six HAM Chamber seismic isolation systems (one stage six degree of freedom active isolation stages capable of ~200 kg payloads)

bull eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

bull 10 interferometer core optics (test masses folding mirrors beam splitter recycling mirrors)

Relative valuation

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the opportunityLIGO-India Technology gain

Five quadruple stage large optics suspensions systems

Triple stage suspensions for remaining suspended optics

Baffles and beam dumps for controlling scattering and stray radiation

Optical distortion monitors and thermal controlcompensation system for large optics

Photo-detectors conditioning electronics actuation electronics and conditioning

Data conditioning and acquisition system software for data acquisition

Supervisory control and monitoring system software for all control systems

Installation tooling and fixturing

Relative valuation

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

In its road-map with a thirty year horizon the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site In what follows this project is referred to as LIGO-India The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community but to broader physics and astronomy research by launching an era of gravitational wave astronomy including the fundamental first direct detection of gravitational waves As the southernmost member observatory of the global array of gravitational wave detectors India would be unique among nations leading the scientific exploration of this new window on the universe The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory It also offers technology that was developed over two decades of highly challenging global RampD effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation amp commissioning Generate amp sustain manpower running for 10 years Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challenges

Trained Manpower for installation amp commissioning

RequirementsFrom LIGO requirements doc

Plans amp Preliminary exploration Sendhil doc

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Indo-US centre for Gravitational Physics and Astronomy

bull Centre of Indo-US Science and Technology Forum (IUSSTF)

bull Exchange program to fund mutual visits and facilitate interaction

bull Nodal centres IUCAA India amp Caltech US

bull Institutions

Indian IUCAA TIFR IISER DU CMI - PI Tarun Souradeep US Caltech WSU - PI Rana Adhikari

APPROVED for funding (Dec 2010)

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challenges

Generate manpower for sustenance of the Intl observatory

Requirements

Plans amp Preliminary exploration

bull Summer internships in Intl labs underwaybull IndIGO schools

ProposalsPost graduate school specialization course

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challengesLarge scale ultra-high Vacuum enclosure

Requirements

Preliminary exploration

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challengesIndian SiteRequirements

Low seismicityLow human generated noiseAir connectivity Acad institution labs industry

Preliminary exploration IISc new campus amp adjoining campuses near Chitra Durga

bull 1hr from Intl airportbull low seismicitybull National science facilities complex plansbull bull

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challengesShort lead time

Requirements

Preliminary exploration

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India hellip the challengesInternation competition

Issues

Preliminary assessment

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-India

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

One is left speculating if by the Centenary of General Relativity in 2015the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of General Relativity

Of all the large scientific projects out there this one is pushing the greatest number of technologies the hardestrdquo

ldquoEvery single technology theyrsquore touching theyrsquore pushing and therersquos a lot of different technologies theyrsquore touchingrdquo

Beverly Berger National Science Foundation Program director for gravitational physics

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

The IndIGO data analysis centre

Tier -2 centre with data archival and computational facilities

Inter-institutional proposal for facility

Propose for a high-throughput Computation and GW Data Archival Centre

Will provide fundamental infrastructure for consolidating GW data analysis expertise in India

Tier 0

bullLIGO Sites at Hanford Livingston

bullData acquisition systems

Tier 1 bullLIGO Labs at Caltech

Tier 2

bullLIGO Lab at MIT LSC institutions like UWM Syracuse etc

bullIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopme

nt

Indian Researchers and Students

TIER3 centres at Univ amp IISERS

Other science groups

Web Services

Collaboration tools

Analysis

LSCLIGO Data

Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre

Courtesy Anand Sengupta

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Primary Science Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 datacompute centre for archival of g-

wave data and analysis Bring together data-analysts within the Indian gravity

wave community Puts IndIGO on the global map for international

collaboration with LIGO Science Collab wide facility Part of LSC participation from IndIGO

100 Tflops = 8500 cores x 3 GHzcoreNeed 8500 cores to carry out a half decent coherent search

for gravitational waves from compact binaries(1 Tflop = 250 GHz = 85 cores x 3 GHz core)

Storage 4x100TB per year per interferometer

Network gigabit backbone National Knowledge Network

Courtesy Anand Sengupta IndIGO

IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wave Observations

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Future GWDA Plans of IndIGO (as part of LSC)

Project leads Sanjit Mitra T Souradeep S Dhurandhar hellip

Extend GW radiometer work (MitraDhurandhar TShellip2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab)

Burst Sources bull Formulationbull Implementation

Courtesy S Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Vetoes for non-Gaussian noise for coherent detection of inspirals

bull Project leads Anand Sengupta Archana Pai M K Harris

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so

Developing a veto for coherent is crucial ndash chi squared

Scope for improving the current chi squared test ndash Japanese collaboration

8th February Delhi Courtesy S Dhurandhar

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Tests of General Relativity using GW observations

Project leads K G Arun Rajesh Nayak and Chandra Kant Mishra Bala Iyer

GWs are unique probes of strong field gravity Their direct detection would enable very precise tests of GR in the dynamical and strong field regime

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods

Possible collaboration with B S Sathyaprakash (Cardiff University) amp P Ajith (Caltech)

Courtesy S Dhurandhar

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Summary (amp next steps)

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

THE END

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

LIGO-Australia Idea and Opportunity

bull The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site W Australia to maximize science benefits like baseline pointing duty cycle technology development and international collaboration

bull The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity

- Indian contribution in hardware (end station vacuum system and controls) Data centre manpower for installation and commissioning

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

Indo-AusMeeting Delhi Feb 2011

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77

• LIGO-India Detecting Einsteinrsquos Elusive Waves Opening a New Wi
• Slide 2
• Space Time as a fabric
• Slide 4
• Slide 5
• Slide 6
• Slide 7
• Slide 8
• Slide 9
• Slide 10
• Slide 11
• Slide 12
• Slide 13
• Slide 14
• GW Astronomy with Intl Network of GW Observatories
• A Century of Waiting
• Gravitational Waves Exist
• Laser Interferometric Gravitational Wave Detectors
• Change in Length manifests as Change in Transmitted Light
• Slide 20
• LIGO and Virgo TODAY
• Expected Annual Coalescence Rates
• Laser Interferometer GW Observatory
• Schematic Optical Design of Advanced LIGO detectors
• Slide 25
• Slide 26
• INDIGO the goals
• Slide 28
• Slide 29
• Slide 30
• LIGO-India Why is it a good idea for India
• LIGO-India Why is it a good idea hellip for the World
• Slide 33
• Slide 34
• Slide 35
• Slide 36
• Slide 37
• Slide 38
• Slide 39
• Slide 40
• Slide 41
• Slide 42
• Slide 43
• Slide 44
• Slide 45
• Slide 46
• Slide 47
• Slide 48
• Slide 49
• Slide 50
• Slide 51
• Slide 52
• Slide 53
• Slide 54
• Slide 55
• Slide 56
• Slide 57
• Slide 58
• Indo-US centre for Gravitational Physics and Astronomy
• Slide 60
• Slide 61
• Slide 62
• Slide 63
• Slide 64
• Slide 65
• Slide 66
• The IndIGO data analysis centre
• Objectives of the data centre
• IndIGO Data CentreIUCAA Indian Initiative in Gravitational-wa
• Future GWDA Plans of IndIGO (as part of LSC)
• Vetoes for non-Gaussian noise for coherent detection of inspir
• Tests of General Relativity using GW observations
• Summary (amp next steps)
• Slide 74
• Slide 75
• Slide 76
• Slide 77