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Fundamental Physics through Fundamental Physics through AstrophysicsAstrophysics

Fundamental Physics through Fundamental Physics through AstrophysicsAstrophysicsChristopher StubbsChristopher Stubbs

Melissa FranklinMelissa Franklin

John OliverJohn Oliver

James BattatJames Battat

Daniel ShermanDaniel Sherman

Ned HenryNed Henry

Michael Wood-VaseyMichael Wood-Vasey

Arti GargArti Garg

Gajus MiknaitisGajus Miknaitis

Malcolm HickenMalcolm Hicken

Christopher StubbsChristopher Stubbs

Melissa FranklinMelissa Franklin

John OliverJohn Oliver

James BattatJames Battat

Daniel ShermanDaniel Sherman

Ned HenryNed Henry

Michael Wood-VaseyMichael Wood-Vasey

Arti GargArti Garg

Gajus MiknaitisGajus Miknaitis

Malcolm HickenMalcolm Hicken

                                                 

Structure of Today’s Structure of Today’s presentationspresentations

Structure of Today’s Structure of Today’s presentationspresentations

Introduction and OverviewIntroduction and Overview StubbsStubbs

Fundamental Gravity: LLR BattatFundamental Gravity: LLR Battat

Dark Energy ScienceDark Energy Science

LSSTLSST StubbsStubbs

Galaxy ClustersGalaxy Clusters StubbsStubbs

PISCO cryo/thermalPISCO cryo/thermal HenryHenry

Introduction and OverviewIntroduction and Overview StubbsStubbs

Fundamental Gravity: LLR BattatFundamental Gravity: LLR Battat

Dark Energy ScienceDark Energy Science

LSSTLSST StubbsStubbs

Galaxy ClustersGalaxy Clusters StubbsStubbs

PISCO cryo/thermalPISCO cryo/thermal HenryHenry

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Emergence of a Standard CosmologyEmergence of a Standard CosmologyEmergence of a Standard CosmologyEmergence of a Standard Cosmology

Our geometrically flat Universe started in a hot big bang Our geometrically flat Universe started in a hot big bang 13.7 Gyrs ago.13.7 Gyrs ago.

The evolution of the Universe is increasingly dominated by The evolution of the Universe is increasingly dominated by the phenomenology of the vacuum. the phenomenology of the vacuum.

Matter, mostly non-baryonic, Matter, mostly non-baryonic, is a minor component. is a minor component.

Luminous matter comprises Luminous matter comprises a preposterously low fraction a preposterously low fraction of the mass of the Universe. of the mass of the Universe.

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Focus is shifting…Focus is shifting…Focus is shifting…Focus is shifting…10 years ago10 years ago

What’s the Dark Matter?What are the values of the cosmological

parameters ( q0, H0)? What’s the connection between primordial

fluctuations and observed large scale structure?

10 years ago10 years agoWhat’s the Dark Matter?What are the values of the cosmological

parameters ( q0, H0)? What’s the connection between primordial

fluctuations and observed large scale structure?

NowNow– What’s the Dark Matter?What’s the Dark Matter?– What physics is responsible for nonzero What physics is responsible for nonzero ??– What’s the connection between primordial fluctuations, What’s the connection between primordial fluctuations,

dark matter, and observed galactic structure?dark matter, and observed galactic structure?– How can we probe the foundations of gravity?How can we probe the foundations of gravity?

NowNow– What’s the Dark Matter?What’s the Dark Matter?– What physics is responsible for nonzero What physics is responsible for nonzero ??– What’s the connection between primordial fluctuations, What’s the connection between primordial fluctuations,

dark matter, and observed galactic structure?dark matter, and observed galactic structure?– How can we probe the foundations of gravity?How can we probe the foundations of gravity?

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Astrophysical Evidence Astrophysical Evidence for New Physicsfor New Physics

Astrophysical Evidence Astrophysical Evidence for New Physicsfor New Physics

Matter-antimatter asymmetry • Baryon number & CP violation in early universe?

Non-baryonic Dark Matter • New particle physics sector?

Neutrino oscillations, mass constraints• Non-zero masses, mixing/oscillations

Non-zero Cosmological Constant, • Evidence for weirdness in the vacuum• Puzzle #1: why is so small?• Puzzle #2: why is so large?

Matter-antimatter asymmetry • Baryon number & CP violation in early universe?

Non-baryonic Dark Matter • New particle physics sector?

Neutrino oscillations, mass constraints• Non-zero masses, mixing/oscillations

Non-zero Cosmological Constant, • Evidence for weirdness in the vacuum• Puzzle #1: why is so small?• Puzzle #2: why is so large?

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Theoretical Context is EvolvingTheoretical Context is EvolvingTheoretical Context is EvolvingTheoretical Context is Evolving• Stringy ideas may produce observable effects Stringy ideas may produce observable effects

• Growing appreciation of the importance of the Growing appreciation of the importance of the gravitational sectorgravitational sector

• Speculative models for Speculative models for -physics, some even -physics, some even falsifiablefalsifiable

• Even in the absence of the evidence for cosmic Even in the absence of the evidence for cosmic acceleration, this would motivate testing acceleration, this would motivate testing gravitational physics on gravitational physics on all all accessible length accessible length scalesscales

• Stringy ideas may produce observable effects Stringy ideas may produce observable effects

• Growing appreciation of the importance of the Growing appreciation of the importance of the gravitational sectorgravitational sector

• Speculative models for Speculative models for -physics, some even -physics, some even falsifiablefalsifiable

• Even in the absence of the evidence for cosmic Even in the absence of the evidence for cosmic acceleration, this would motivate testing acceleration, this would motivate testing gravitational physics on gravitational physics on all all accessible length accessible length scalesscales

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Through some profound but not yet understood mechanism, the

vacuum energy must be cancelled to arrive at value of identically zero ummm... Supersymmetry uhhh ...Planck Mass

...

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Dark MatterDark Matter• CMBCMB• MicrolensingMicrolensing• Cosmic Cosmic

structuresstructures

• Direct detection?Direct detection?

Dark MatterDark Matter• CMBCMB• MicrolensingMicrolensing• Cosmic Cosmic

structuresstructures

• Direct detection?Direct detection?

Dark EnergyDark Energy

• SNeSNe• ClustersClusters

• Next generNext gener.

Dark EnergyDark Energy

• SNeSNe• ClustersClusters

• Next generNext gener. Precision Precision

TestsTests

• AMOAMO• gravitygravity

Precision Precision TestsTests

• AMOAMO• gravitygravity

High Energy High Energy CollisionsCollisions

• LHCLHC• NeutrinosNeutrinos

High Energy High Energy CollisionsCollisions

• LHCLHC• NeutrinosNeutrinos

Fundamental Physics is a Departmental PriorityFundamental Physics is a Departmental PriorityFundamental Physics is a Departmental PriorityFundamental Physics is a Departmental Priority

• One of 3 focus areas for physics Department’s strategic planOne of 3 focus areas for physics Department’s strategic plan

• Joint experimental/theory outlookJoint experimental/theory outlook

• 2004/2005: Search for junior faculty in fundamental astrophysics2004/2005: Search for junior faculty in fundamental astrophysics

• Offer to Doug Finkbeiner, now at Princeton, accepted

• Initial 100% appointment in astronomy, then we’ll see…

Laboratory for Particle Physics and Cosmology (LPPC) will be the Laboratory for Particle Physics and Cosmology (LPPC) will be the

experimental component of this effort. experimental component of this effort.

• One of 3 focus areas for physics Department’s strategic planOne of 3 focus areas for physics Department’s strategic plan

• Joint experimental/theory outlookJoint experimental/theory outlook

• 2004/2005: Search for junior faculty in fundamental astrophysics2004/2005: Search for junior faculty in fundamental astrophysics

• Offer to Doug Finkbeiner, now at Princeton, accepted

• Initial 100% appointment in astronomy, then we’ll see…

Laboratory for Particle Physics and Cosmology (LPPC) will be the Laboratory for Particle Physics and Cosmology (LPPC) will be the

experimental component of this effort. experimental component of this effort.

Fundamental AstrophysicsFundamental AstrophysicsFundamental AstrophysicsFundamental Astrophysics

Exploiting the tools and techniques of Exploiting the tools and techniques of astrophysics to address fundamental physics astrophysics to address fundamental physics issues - an extension of existing programissues - an extension of existing program

Laboratory for Particle PhysicsLaboratory for Particle Physics and Cosmologyand Cosmology

Exploiting the tools and techniques of Exploiting the tools and techniques of astrophysics to address fundamental physics astrophysics to address fundamental physics issues - an extension of existing programissues - an extension of existing program

Laboratory for Particle PhysicsLaboratory for Particle Physics and Cosmologyand Cosmology

GravityGravity

Particle physicsParticle physics

CosmologyCosmology

11Carroll, astro-ph/0004075

A Repulsive Result!A Repulsive Result!

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Two philosophically distinct possibilitiesTwo philosophically distinct possibilities......Two philosophically distinct possibilitiesTwo philosophically distinct possibilities......

• A “classical” cosmological constant, A “classical” cosmological constant, as envisioned by Einstein, residing as envisioned by Einstein, residing in the gravitational sector. in the gravitational sector.

• A “Vacuum energy” effect, arising A “Vacuum energy” effect, arising from quantum fluctuations in the from quantum fluctuations in the vacuum, acting as a “source” termvacuum, acting as a “source” term

• A “classical” cosmological constant, A “classical” cosmological constant, as envisioned by Einstein, residing as envisioned by Einstein, residing in the gravitational sector. in the gravitational sector.

• A “Vacuum energy” effect, arising A “Vacuum energy” effect, arising from quantum fluctuations in the from quantum fluctuations in the vacuum, acting as a “source” termvacuum, acting as a “source” term

In either case, it’s new fundamental physics!In either case, it’s new fundamental physics!

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Dark Energy’s Equation of StateDark Energy’s Equation of StateDark Energy’s Equation of StateDark Energy’s Equation of State w = 0, matter

P = w w = 1/3 ,radiation

w = 1, w = N/3, topological defects

w = 0, matter

P = w w = 1/3 ,radiation

w = 1, w = N/3, topological defects

3 3(1 )

0 0

(1 )( ) (1 )(1 ) (1 )

zw

L

c zD z z z dz

H+

+ ′ ′ ′= − + + +∫

For a flat Universe, luminosity For a flat Universe, luminosity distance depends only upon z, distance depends only upon z, , w., w.

(assumes w is constant) (assumes w is constant)

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Equation of State DependenceEquation of State DependenceEquation of State DependenceEquation of State Dependence

Difference in apparent SN brightness vs. zDifference in apparent SN brightness vs. z=0.73, flat cosmology=0.73, flat cosmology

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High-Z SN Team Results High-Z SN Team Results High-Z SN Team Results High-Z SN Team Results

Tonry et al (2003)

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Sure looks a lot like w=Sure looks a lot like w=11Sure looks a lot like w=Sure looks a lot like w=11

For For w(z) = ww(z) = w00 + w`z + w`z, w` = dw/dz|, w` = dw/dz|z=0z=0For For w(z) = ww(z) = w00 + w`z + w`z, w` = dw/dz|, w` = dw/dz|z=0z=0

Reiss et al

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Importance of non-zero Importance of non-zero . . Importance of non-zero Importance of non-zero . .

• If true, this is clear evidence for new If true, this is clear evidence for new physics at an interface we don’t physics at an interface we don’t presently understandpresently understand

• Most recent shift in cosmological Most recent shift in cosmological paradigm:paradigm:

• Heliocentric • Big Bang • Dark Matter >> luminous/baryonic matter• Inflationary paradigm• Dark Energy >> Dark matter >> luminous material

• If true, this is clear evidence for new If true, this is clear evidence for new physics at an interface we don’t physics at an interface we don’t presently understandpresently understand

• Most recent shift in cosmological Most recent shift in cosmological paradigm:paradigm:

• Heliocentric • Big Bang • Dark Matter >> luminous/baryonic matter• Inflationary paradigm• Dark Energy >> Dark matter >> luminous material

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Has non-zero Has non-zero toppled reductionism!? toppled reductionism!?Has non-zero Has non-zero toppled reductionism!? toppled reductionism!?• The reductionist approach to physics The reductionist approach to physics

has been very successfulhas been very successful• Newton’s Universal law of gravitation• Atoms, Electricity & Magnetism• Quarks and Leptons• Unification of fundamental interactions...

• The reductionist approach to physics The reductionist approach to physics has been very successfulhas been very successful

• Newton’s Universal law of gravitation• Atoms, Electricity & Magnetism• Quarks and Leptons• Unification of fundamental interactions...

mmee

mmtoptop

FF= 0= 0

Elegant TOE equationElegant TOE equation

The goal:The goal:

Constrained parametersConstrained parameters

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Two possible “natural” values Two possible “natural” values Two possible “natural” values Two possible “natural” values

• Vacuum energy integrated up to Planck Vacuum energy integrated up to Planck scale scale

• Cancellation via tooth fairy:Cancellation via tooth fairy:

• But it’s measured to be around 0.7!But it’s measured to be around 0.7!

• Vacuum energy integrated up to Planck Vacuum energy integrated up to Planck scale scale

• Cancellation via tooth fairy:Cancellation via tooth fairy:

• But it’s measured to be around 0.7!But it’s measured to be around 0.7!

12010 :

0.0000000000000000000000000000.... =

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From string theory perspective...From string theory perspective...From string theory perspective...From string theory perspective...

• Constraining Constraining =0 reduces number of =0 reduces number of candidate vacuum configurations candidate vacuum configurations (“landscapes”).(“landscapes”).

• With non-zero With non-zero , get of order 10, get of order 1010001000 landscapes, each with potentially different landscapes, each with potentially different kinds of physicskinds of physics

• What picks the one we inhabit? What picks the one we inhabit?

• Constraining Constraining =0 reduces number of =0 reduces number of candidate vacuum configurations candidate vacuum configurations (“landscapes”).(“landscapes”).

• With non-zero With non-zero , get of order 10, get of order 1010001000 landscapes, each with potentially different landscapes, each with potentially different kinds of physicskinds of physics

• What picks the one we inhabit? What picks the one we inhabit?

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The “selection effect” viewpointThe “selection effect” viewpointThe “selection effect” viewpointThe “selection effect” viewpoint• From all possible (presumably equally likely) From all possible (presumably equally likely)

sets of parameters and interaction strengths, sets of parameters and interaction strengths, only a small subset could produce heavy only a small subset could produce heavy elements and evolve life.elements and evolve life.

• This selection effect is what determines This selection effect is what determines

observables, such as mobservables, such as mee/m/mpp, coupling strengths, , coupling strengths, etc, and etc, and notnot something deep and fundamental! something deep and fundamental!

Ouch.Ouch.

• From all possible (presumably equally likely) From all possible (presumably equally likely) sets of parameters and interaction strengths, sets of parameters and interaction strengths, only a small subset could produce heavy only a small subset could produce heavy elements and evolve life.elements and evolve life.

• This selection effect is what determines This selection effect is what determines

observables, such as mobservables, such as mee/m/mpp, coupling strengths, , coupling strengths, etc, and etc, and notnot something deep and fundamental! something deep and fundamental!

Ouch.Ouch.

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Understanding the Fundamental Physics of Understanding the Fundamental Physics of Dark Energy is a Major PriorityDark Energy is a Major Priority

Understanding the Fundamental Physics of Understanding the Fundamental Physics of Dark Energy is a Major PriorityDark Energy is a Major Priority

• 2 regimes of current interest:2 regimes of current interest:

1)1) Evolution of cosmic geometry, manifested Evolution of cosmic geometry, manifested in different waysin different ways

2)2) Experimental gravitation, searching for the Experimental gravitation, searching for the next clue….next clue….

We are active on both frontsWe are active on both fronts

• 2 regimes of current interest:2 regimes of current interest:

1)1) Evolution of cosmic geometry, manifested Evolution of cosmic geometry, manifested in different waysin different ways

2)2) Experimental gravitation, searching for the Experimental gravitation, searching for the next clue….next clue….

We are active on both frontsWe are active on both fronts

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James, LLRJames, LLRJames, LLRJames, LLR

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What would an optimized What would an optimized ground-based facility look like?ground-based facility look like?

What would an optimized What would an optimized ground-based facility look like?ground-based facility look like?

• Large collecting area Large collecting area

• Wide field of viewWide field of view

• Real-time analysis of dataReal-time analysis of data

• Significant leap in figure-of-meritSignificant leap in figure-of-meritArea x Field of View

• Large collecting area Large collecting area

• Wide field of viewWide field of view

• Real-time analysis of dataReal-time analysis of data

• Significant leap in figure-of-meritSignificant leap in figure-of-meritArea x Field of View

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Large Synoptic Survey TelescopeLarge Synoptic Survey TelescopeLarge Synoptic Survey TelescopeLarge Synoptic Survey TelescopeHighly ranked in Decadal SurveyHighly ranked in Decadal Survey

Optimized for time domainOptimized for time domain

scan modescan mode

deep modedeep mode

9.6 square degree field9.6 square degree field

6.5m effective aperture6.5m effective aperture

24th mag in 20 sec24th mag in 20 sec

> 5 Tbyte/night> 5 Tbyte/night

Real-time analysisReal-time analysis

Simultaneous multiple science goalsSimultaneous multiple science goals

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So Why Should So Why Should Physicists Physicists Care About the Large Care About the Large

Synoptic Survey Synoptic Survey Telescope?Telescope?

So Why Should So Why Should Physicists Physicists Care About the Large Care About the Large

Synoptic Survey Synoptic Survey Telescope?Telescope?

Fundamental Physics via AstrophysicsFundamental Physics via Astrophysics• Nature of Dark Matter (strong, weak and Nature of Dark Matter (strong, weak and lensing)lensing)• Dark Energy (SNe, lensing, Large Scale Structure)Dark Energy (SNe, lensing, Large Scale Structure)• Extreme Systems (linkages with LISA, EXIST…)Extreme Systems (linkages with LISA, EXIST…)

Qualitative leap in capabilities (AQualitative leap in capabilities (A product) product)

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Some ExamplesSome ExamplesSome ExamplesSome Examples• Thousands of type Ia supernovaeThousands of type Ia supernovae

Detailed study of physics Isotropy of Hubble diagram Subdivide data set

• Host galaxy type• Redshift shells• SN color/decline parameter

• Time delays from strongly lensed SNeTime delays from strongly lensed SNe Constrains nature of dark matter

• Weak Lensing of galaxies as a probe of evolution of Weak Lensing of galaxies as a probe of evolution of structurestructure

• Optical counterparts to gravity wave sourcesOptical counterparts to gravity wave sources Break degeneracy in (1+z)Mchirp

• Thousands of type Ia supernovaeThousands of type Ia supernovae Detailed study of physics Isotropy of Hubble diagram Subdivide data set

• Host galaxy type• Redshift shells• SN color/decline parameter

• Time delays from strongly lensed SNeTime delays from strongly lensed SNe Constrains nature of dark matter

• Weak Lensing of galaxies as a probe of evolution of Weak Lensing of galaxies as a probe of evolution of structurestructure

• Optical counterparts to gravity wave sourcesOptical counterparts to gravity wave sources Break degeneracy in (1+z)Mchirp

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LSST ChallengesLSST ChallengesLSST ChallengesLSST Challenges

• Large effective aperture wide field telescopeLarge effective aperture wide field telescope

• 3 Gpix focal plane3 Gpix focal plane

• Analysis pipelineAnalysis pipeline

• Automated Variability ClassificationAutomated Variability Classification

• Database schema/structure and indexingDatabase schema/structure and indexing

• Large effective aperture wide field telescopeLarge effective aperture wide field telescope

• 3 Gpix focal plane3 Gpix focal plane

• Analysis pipelineAnalysis pipeline

• Automated Variability ClassificationAutomated Variability Classification

• Database schema/structure and indexingDatabase schema/structure and indexing

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Harvard LPPC LSST TasksHarvard LPPC LSST TasksHarvard LPPC LSST TasksHarvard LPPC LSST Tasks

As part of the joint effort for DOE contribution to LSST, we are As part of the joint effort for DOE contribution to LSST, we are engaged in three main tasks:engaged in three main tasks:

1)1) Camera readout electronics: J. Oliver and teamCamera readout electronics: J. Oliver and team

2)2) System calibration: Stubbs and students System calibration: Stubbs and students

3)3) Detector optimization and characterization: Oliver, StubbsDetector optimization and characterization: Oliver, Stubbs

Overall DOE effort on camera project managed by SLACOverall DOE effort on camera project managed by SLAC

We have close working relationship with BNL colleagues We have close working relationship with BNL colleagues

As part of the joint effort for DOE contribution to LSST, we are As part of the joint effort for DOE contribution to LSST, we are engaged in three main tasks:engaged in three main tasks:

1)1) Camera readout electronics: J. Oliver and teamCamera readout electronics: J. Oliver and team

2)2) System calibration: Stubbs and students System calibration: Stubbs and students

3)3) Detector optimization and characterization: Oliver, StubbsDetector optimization and characterization: Oliver, Stubbs

Overall DOE effort on camera project managed by SLACOverall DOE effort on camera project managed by SLAC

We have close working relationship with BNL colleagues We have close working relationship with BNL colleagues

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Recent LSST ProgressRecent LSST ProgressRecent LSST ProgressRecent LSST Progress

• NSF funding for D & D imminent (next 2 weeks?)NSF funding for D & D imminent (next 2 weeks?)

• Conceptual design for front end electronics under wayConceptual design for front end electronics under way

• Risk reduction through early detector development/assessmentRisk reduction through early detector development/assessment

• Successful trial run on calibration technique, 1/05Successful trial run on calibration technique, 1/05

• Primary mirror contract issuedPrimary mirror contract issued

• Site selection well under waySite selection well under way

• Full management structure now in placeFull management structure now in place

• NSF funding for D & D imminent (next 2 weeks?)NSF funding for D & D imminent (next 2 weeks?)

• Conceptual design for front end electronics under wayConceptual design for front end electronics under way

• Risk reduction through early detector development/assessmentRisk reduction through early detector development/assessment

• Successful trial run on calibration technique, 1/05Successful trial run on calibration technique, 1/05

• Primary mirror contract issuedPrimary mirror contract issued

• Site selection well under waySite selection well under way

• Full management structure now in placeFull management structure now in place

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dd

Timing BusTiming Bus

Data Bus

Controlinterface

Controlinterface Data Card

Cryostat wall

Single ~2.4 Gb/s fiber per

Datacard

•Timing & control interface• “Engineering” data readout• ~ 10^3 total Dewar penetrations

Fiber driver

Multiple CCDs/FEMs

to a Data Card

• Front end cards • Analog signal processing• ~ -100C

• Back end cards • A/D conversion• Control / timing signal transmission • Data collection & transmission• ~ -20C – 0C

Science Array Readout SchemeScience Array Readout SchemeScience Array Readout SchemeScience Array Readout Scheme

33

• “Raft based” electronics packaging scheme• All electronics, front end & back end, must live in < 126 mm x 126 mm footprint • May be “tiled” to accommodate wavefront sensors• 3 x 3 array of 42mm sq sensors• 16 amps per chip x 9 chips = 144 Mega-pixels• 32 rafts x 9 detectors/raft = 288 CCDs

• Heat removal in two zones Front end near sensor temperature: ~ -100C Back end near zero: ~ -20C to 0C

Electronics PackagingElectronics PackagingElectronics PackagingElectronics Packaging

34

Minimal circuitry for each CCD port (x 288 per raft) • 16-bit 2 Ms/s ADC• Differential amplifier to drive ADC

Backend Electronics packaging

ADC

AD8138 AD7677

“chip scale” 7mm x 7mm package

3mm x 3mm (plus pins) SOIC

From front end

35

Backend Electronics packaging

• 8 complete circuits can be packaged on a 40mm x 60mm carrier card• Cooling path provided by copper core pc board (Target temp -20C to 0C)• 4 ADC cards required per CCD• 36 ADC cards per raft

36

Multi-layer, copper core pcbs from Dynamic Detail Inc.

• ½ mm thick copper core will maintain DT ~ 1C across ADC board• Thermal mass for stability while power cycling

37

Backend Electronics packaging- ADC mother boards -

• 6 ADC cards/mother board (48 ADC channels)• 123 mm x 150 mm• Copper cooling bars

38

Backend Electronics packaging- Backend Module -

• Complete (slave) backend readout system for 288 CCD ports• 123mm x 123 mm x < 200mm tall• “Base” board contains

All local control elements Frame buffers Fiber driver Low speed (engineering) interface

39

Raft based front end / back end electronics package

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Electronics Development- Next steps -

Prototype versions• Front end

Discrete circuits 4-8 channels

• Back end Octal ADC board – “Near final” design, no copper core Test board with locations for 4x Octal ADC boards Flex cable connectors to multiple front end boards On board controller (FPGA, later to migrate to “Timing & Control Card in Timing Control Crate” USB 2.0 data path (1 sec/256 Mb frame buffer)

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Electronics Development- Next step (cont’) -

First phase of front-end / back end development yields• Vacuum compatible front end electronics of 4-8 channels/card• Stand-alone 32 channel controller (1 full LSST sensor)• Designed for all LSST readout specs ( ~5e rms @ 250 kHz, etc) • Testing begins end of 2005• To become available as general “Test stand” for LSST work.

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Camera Grounding Document-P. O’Connor, J. Oliver, V. Radeka, M. Warner -

29-April-05

Purpose• Outline a consistent set of rules for grounding of all electrically operated components within the camera body (including “External Services Crate”• Outline consistent rules for electrical and control cables to such components.• Document to be integrated with further grounding control doc for Telescope & Observatory

Main features• Camera body has very few, but well controlled, external cable connections

Electrical services input One single ethernet cable for slow control/communications (optical preferred) All internal objects addressable via internal ethernet switch (See Camera Control Document) No individual control cabling from Camera objects to outside world. Fiber optic data output only A single ground strap to telescope Preferred mounting to telescope via insulated mounting All other connections to camera must be ground isolated (example: Vacuum lines, cooling lines, cryogenic lines, etc…. )

Status Camera Grounding Document is a proposal which we hope to have accepted for LSST.

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Current Metrology Chain for Ground-Current Metrology Chain for Ground-based Astronomical Flux based Astronomical Flux

Measurements.Measurements.

Current Metrology Chain for Ground-Current Metrology Chain for Ground-based Astronomical Flux based Astronomical Flux

Measurements.Measurements.

Black Body Black Body CalibratorCalibrator

Celestial Celestial SourcesSources

Celestial Celestial Calibrator, Calibrator,

VegaVega

Supernova measurements require knowing Supernova measurements require knowing relative instrumental sensitivity vs. relative instrumental sensitivity vs.

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Vega is primary celestial calibratorVega is primary celestial calibratorVega is primary celestial calibratorVega is primary celestial calibrator

4%

2%

5000 A 1 m

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Detector-based Radiometry Detector-based Radiometry Detector-based Radiometry Detector-based Radiometry

Modern Modern metrology for metrology for

radiometric radiometric measurements measurements

is based on is based on detectors, not detectors, not

sources. sources.

Modern Modern metrology for metrology for

radiometric radiometric measurements measurements

is based on is based on detectors, not detectors, not

sources. sources.

Larson, Bruce and Parr, NIST special publication 250-41Larson, Bruce and Parr, NIST special publication 250-41

46

Transferring flux standard to Transferring flux standard to photodiodesphotodiodes

Transferring flux standard to Transferring flux standard to photodiodesphotodiodes

Through 1 intermediate step, this Through 1 intermediate step, this calibration is transferred to Si calibration is transferred to Si photodiodesphotodiodes

Through 1 intermediate step, this Through 1 intermediate step, this calibration is transferred to Si calibration is transferred to Si photodiodesphotodiodes

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An alternative calibration approachAn alternative calibration approachAn alternative calibration approachAn alternative calibration approachCalibrate end-to-end relative system response Calibrate end-to-end relative system response

primaryprimarycorrector opticscorrector opticsfilterfilterdetectordetector

relative to Si photodiode. relative to Si photodiode.

10% 10%

Opotek tunable laserOpotek tunable laser~100 mW~100 mW

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LSST summaryLSST summaryLSST summaryLSST summary

• Harvard is a key participantHarvard is a key participant• Science: Dark energy & Dark matter• Technical: Oliver = lead on camera electronics• Management: Stubbs on Science Adv. Group

• Substantial progress in past 12 mo.Substantial progress in past 12 mo.• Project has matured, with full mgmt Project has matured, with full mgmt

structure now in placestructure now in place• Preparation of full DOE proposal under Preparation of full DOE proposal under

way, in final revision stage. way, in final revision stage.

• Harvard is a key participantHarvard is a key participant• Science: Dark energy & Dark matter• Technical: Oliver = lead on camera electronics• Management: Stubbs on Science Adv. Group

• Substantial progress in past 12 mo.Substantial progress in past 12 mo.• Project has matured, with full mgmt Project has matured, with full mgmt

structure now in placestructure now in place• Preparation of full DOE proposal under Preparation of full DOE proposal under

way, in final revision stage. way, in final revision stage.

49

Cosmology from SZ Clusters:Cosmology from SZ Clusters:Parallel Imager for Southern Cosmological Observations Parallel Imager for Southern Cosmological Observations

(PISCO)(PISCO)

Cosmology from SZ Clusters:Cosmology from SZ Clusters:Parallel Imager for Southern Cosmological Observations Parallel Imager for Southern Cosmological Observations

(PISCO)(PISCO)• Multiple projects now funded and under way to use Multiple projects now funded and under way to use

SZ effect to detect galaxy clusters, down to ~2 SZ effect to detect galaxy clusters, down to ~2 xx 10 101414 MMsolarsolar

• Expectation is ~ 7 clusters per sq degreeExpectation is ~ 7 clusters per sq degree• South Pole Telescope will map 4000 sq deg; 29,000 clusters

• SZ signal strength z-independentSZ signal strength z-independent • Optical observations needed for zOptical observations needed for z

• Spectroscopy – SALT • Wide field multiband survey – DEC 2009 • Targeted moderate field multiband observations – our approach!

• Multiple projects now funded and under way to use Multiple projects now funded and under way to use SZ effect to detect galaxy clusters, down to ~2 SZ effect to detect galaxy clusters, down to ~2 xx 10 101414 MMsolarsolar

• Expectation is ~ 7 clusters per sq degreeExpectation is ~ 7 clusters per sq degree• South Pole Telescope will map 4000 sq deg; 29,000 clusters

• SZ signal strength z-independentSZ signal strength z-independent • Optical observations needed for zOptical observations needed for z

• Spectroscopy – SALT • Wide field multiband survey – DEC 2009 • Targeted moderate field multiband observations – our approach!

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Conceptual DesignConceptual DesignConceptual DesignConceptual Design

Pass Pass > 7000 A> 7000 A

Pass Pass > 5500 A> 5500 A

Pass Pass > 8500 A> 8500 A

ii

zz

rr

gg

Common Common shuttershutter

51

Pan-Starrs bandsPan-Starrs bandsPan-Starrs bandsPan-Starrs bands

g r i z y

4000 A break at z of 0.2 0.5 0.8 1.0 1.25 1.5

52

CollaboratorsCollaboratorsCollaboratorsCollaborators

• Christopher Stubbs, CfA & LPPCChristopher Stubbs, CfA & LPPC• Melissa Franklin, LPPCMelissa Franklin, LPPC• Tony Stark, CfATony Stark, CfA• John Geary, CfAJohn Geary, CfA• James Battat, LPPCJames Battat, LPPC• Ned Henry, LPPCNed Henry, LPPC• South Pole Telescope/Dark Energy Survey collaboration: South Pole Telescope/Dark Energy Survey collaboration: • J. Carlstrom (Chicago), J. Mohr (Illinois)...J. Carlstrom (Chicago), J. Mohr (Illinois)...

• Christopher Stubbs, CfA & LPPCChristopher Stubbs, CfA & LPPC• Melissa Franklin, LPPCMelissa Franklin, LPPC• Tony Stark, CfATony Stark, CfA• John Geary, CfAJohn Geary, CfA• James Battat, LPPCJames Battat, LPPC• Ned Henry, LPPCNed Henry, LPPC• South Pole Telescope/Dark Energy Survey collaboration: South Pole Telescope/Dark Energy Survey collaboration: • J. Carlstrom (Chicago), J. Mohr (Illinois)...J. Carlstrom (Chicago), J. Mohr (Illinois)...

53

South Pole Telescope (SPT) SurveySouth Pole Telescope (SPT) SurveySouth Pole Telescope (SPT) SurveySouth Pole Telescope (SPT) Survey

• Bolometric focal plane, 1000 Bolometric focal plane, 1000 elements, and 10m aperture elements, and 10m aperture telescope. telescope.

• Will map Southern Will map Southern extragalactic skyextragalactic sky

• RA from 20 hrs to 7 hrs• DEC from –30 to –75 degrees

• Currently funded by NSF Currently funded by NSF polar programs, under polar programs, under constructionconstruction

• Early 2007 first light. Early 2007 first light.

• Bolometric focal plane, 1000 Bolometric focal plane, 1000 elements, and 10m aperture elements, and 10m aperture telescope. telescope.

• Will map Southern Will map Southern extragalactic skyextragalactic sky

• RA from 20 hrs to 7 hrs• DEC from –30 to –75 degrees

• Currently funded by NSF Currently funded by NSF polar programs, under polar programs, under constructionconstruction

• Early 2007 first light. Early 2007 first light.

54

Anticipated Cluster z-distributionAnticipated Cluster z-distributionAnticipated Cluster z-distributionAnticipated Cluster z-distribution

90% within z<1.290% within z<1.2

50% within z<0.550% within z<0.5

Carlstrom, Holder and ReeseCarlstrom, Holder and ReeseAnn Rev Astron AstrophysAnn Rev Astron Astrophys, 2002, 2002

55

Photometric Redshift for ClustersPhotometric Redshift for ClustersPhotometric Redshift for ClustersPhotometric Redshift for Clusters

• Photo-z’s for individual galaxies tend to have Photo-z’s for individual galaxies tend to have scatter of scatter of zz/(1+z)~0.03, but with a few /(1+z)~0.03, but with a few “catastrophic” outliers. “catastrophic” outliers.

• Combination of morphology, magnitude, color Combination of morphology, magnitude, color and location can be used to establish and location can be used to establish cluster’s redshift. cluster’s redshift.

• Robust statistics can be used to eliminate Robust statistics can be used to eliminate “outliers”.“outliers”.

• Photo-z’s for individual galaxies tend to have Photo-z’s for individual galaxies tend to have scatter of scatter of zz/(1+z)~0.03, but with a few /(1+z)~0.03, but with a few “catastrophic” outliers. “catastrophic” outliers.

• Combination of morphology, magnitude, color Combination of morphology, magnitude, color and location can be used to establish and location can be used to establish cluster’s redshift. cluster’s redshift.

• Robust statistics can be used to eliminate Robust statistics can be used to eliminate “outliers”.“outliers”.

56

Photometric Redshifts in SDSS bandsPhotometric Redshifts in SDSS bandsPhotometric Redshifts in SDSS bandsPhotometric Redshifts in SDSS bands

Blanton et al, astro-ph/0205243Blanton et al, astro-ph/0205243

57

Early-type galaxies in SDSS bandsEarly-type galaxies in SDSS bandsEarly-type galaxies in SDSS bandsEarly-type galaxies in SDSS bands

g-r 0.7g-r 0.7

r-i 0.3r-i 0.3

r-z 0.8r-z 0.8

g-r 0.7g-r 0.7

r-i 0.3r-i 0.3

r-z 0.8r-z 0.8

Bernardi et al, astro-ph/031629Bernardi et al, astro-ph/031629

g 20.7g 20.7r 20.0r 20.0i 19.7i 19.7z 19.2z 19.2

58 Brodwin et al, astro-ph/0310038

Relevant Magnitudes are 18<r<24Relevant Magnitudes are 18<r<24Relevant Magnitudes are 18<r<24Relevant Magnitudes are 18<r<24

59

m ABm AB gg rr ii zz Median redshiftMedian redshift

(r mag)(r mag)

2323 3535 8686 320320 870870 0.52 to 230.52 to 23rdrd

23.523.5 7878 210210 800800 22002200 0.730.73

2424 180180 500500 19001900 55005500 0.850.85

24.524.5 450450 12001200 49004900 1300013000 1.011.01

Time (sec) to reach SNR=10 Time (sec) to reach SNR=10 Extended source, ABmag in 2.2 arcsec apertureExtended source, ABmag in 2.2 arcsec apertureDark time, 0.8 arcsec, airmass=1.2, scaled to Magellan and high-Dark time, 0.8 arcsec, airmass=1.2, scaled to Magellan and high-http://rpm.cfht.hawaii.edu/~megacam/diet/DIET.rpm

Galaxy colors roughly follow contours of constant integration Galaxy colors roughly follow contours of constant integration

Shaded boxes are DEC target 10Shaded boxes are DEC target 10 magnitudes. magnitudes.

We should get ½ the clusters (those with z<0.5) in 60 secWe should get ½ the clusters (those with z<0.5) in 60 sec

60

Clusters per unit telescope timeClusters per unit telescope timeClusters per unit telescope timeClusters per unit telescope timeZ rangeZ range NN Time (seconds)Time (seconds)

0 – 0.20 – 0.2 1515 15*60 = 90015*60 = 900

0.2 – 0.40.2 – 0.4 30 30 30*60 = 180030*60 = 1800

0.4 – 0.60.4 – 0.6 30 30 30*60 = 180030*60 = 1800

0.6 – 0.80.6 – 0.8 1515 15*200 = 300015*200 = 3000

0.8 – 1.00.8 – 1.0 1010 10*600 = 600010*600 = 6000

1.0 – 1.21.0 – 1.2 99

1.2 – 1.41.2 – 1.4 44 15*1000= 1500015*1000= 15000

1.4 – 1.61.4 – 1.6 22

totalstotals 115115 ~4 hrs for 100, z<1~4 hrs for 100, z<1

4.2 hours for 15 more, z>14.2 hours for 15 more, z>1

61

Return on Magellan Time InvestmentReturn on Magellan Time InvestmentReturn on Magellan Time InvestmentReturn on Magellan Time Investment

Could get 200 clusters out to z~1, or 100 Could get 200 clusters out to z~1, or 100 clusters out to z of 1.5, in 1 night.clusters out to z of 1.5, in 1 night.

Fifteen dark nights on Magellan could Fifteen dark nights on Magellan could produce photo-z’s for 3000 clusters out produce photo-z’s for 3000 clusters out to z=1, about 10% of the total expected to z=1, about 10% of the total expected from SPT. from SPT.

Could get 200 clusters out to z~1, or 100 Could get 200 clusters out to z~1, or 100 clusters out to z of 1.5, in 1 night.clusters out to z of 1.5, in 1 night.

Fifteen dark nights on Magellan could Fifteen dark nights on Magellan could produce photo-z’s for 3000 clusters out produce photo-z’s for 3000 clusters out to z=1, about 10% of the total expected to z=1, about 10% of the total expected from SPT. from SPT.

Angle-dependence of Dichroic Angle-dependence of Dichroic TransmissionTransmission

Angle-dependence of Dichroic Angle-dependence of Dichroic TransmissionTransmission

Although light is collimated, different parts of imaged Although light is collimated, different parts of imaged field send rays through the system at different anglesfield send rays through the system at different angles

Angle-of-incidence dependence of beam splitters Angle-of-incidence dependence of beam splitters produces color gradients across fieldproduces color gradients across field

Although light is collimated, different parts of imaged Although light is collimated, different parts of imaged field send rays through the system at different anglesfield send rays through the system at different angles

Angle-of-incidence dependence of beam splitters Angle-of-incidence dependence of beam splitters produces color gradients across fieldproduces color gradients across field

30 degrees Incidence

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

350 450 550 650 750 850 950 1050Wavelength (nm)

Transmission

g

r

i

z

24 degrees Incidence

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

350 450 550 650 750 850 950 1050Wavelength (nm)

Transmission

g

r

i

z

Ned!Ned!

64

SetupSetupSetupSetup

Six mirrors, three dichroics

Equal optical paths

Minimal dichroic angle (11.42 degrees)

Two mirrors, three dichroics

Compact setup

Larger dichroic angle (22.5 degrees)

65

Cryomechanics Inside the Pisco DewarCryomechanics Inside the Pisco DewarCryomechanics Inside the Pisco DewarCryomechanics Inside the Pisco Dewar

o Mechanical mounting of CCD within dewar

o Cooling and precise thermal control of CCD

o Electronics for handling CCD output

o Fitting this together efficiently into an easily mountable unit

66

Window EndWindow EndWindow EndWindow End

• Light enters the dewar through a window lens, focusing light onto the CCDs

• There are two CCDs on each focal plane, mounted on a round metal plate

• The CCD plate is held off from the flange by a rigid hexapod structure of 3/16” G-10 rods

67

Thermal ControlThermal ControlThermal ControlThermal Control

CCD plate lightly coupled to outside air Ball bearings separate flange from aluminum ring

Thin 3/16” G-10 rods have low thermal conductivity (.0007 cal/cm-sec-oC)

Copper cold strap attaches CCD plate to Cryotiger cold end

Heat sensor (platinum RTD) and distributed heater (Nichrome wire) on CCD plateLakeshore temperature controller uses tuned PID loop to hold CCD plate at 160 oC

68

ElectronicsElectronicsElectronicsElectronics

The heater and heat sensor power and data The heater and heat sensor power and data lines will come out one 12-pin hermetic lines will come out one 12-pin hermetic connectorconnector

The CCD data will come out a separate, The CCD data will come out a separate, larger hermetic connector directly into a larger hermetic connector directly into a preamp board mounted on the outside of the preamp board mounted on the outside of the flangeflange

Both connectors will fit on the same flange as Both connectors will fit on the same flange as the vacuum pump mounting, saving spacethe vacuum pump mounting, saving space

The heater and heat sensor power and data The heater and heat sensor power and data lines will come out one 12-pin hermetic lines will come out one 12-pin hermetic connectorconnector

The CCD data will come out a separate, The CCD data will come out a separate, larger hermetic connector directly into a larger hermetic connector directly into a preamp board mounted on the outside of the preamp board mounted on the outside of the flangeflange

Both connectors will fit on the same flange as Both connectors will fit on the same flange as the vacuum pump mounting, saving spacethe vacuum pump mounting, saving space

69

5-way cross accommodates two focal planes per cold head

The bottom flange will mount rigidly to an optics table

Although not shown, the far flange will have three hermetic connectors for

electrical throughput (one for each pair of CCDs and one for thermal

control) in addition to a vacuum valve

70

Thermal Prototype Project StatusThermal Prototype Project StatusThermal Prototype Project StatusThermal Prototype Project Status

• We are currently building the final components of a We are currently building the final components of a prototype dewar for thermal testing prototype dewar for thermal testing

• We are already in possession of all the necessary We are already in possession of all the necessary equipment for thermal control of the system equipment for thermal control of the system (temperature controller, cooling system, vacuum (temperature controller, cooling system, vacuum fittings, etc.)fittings, etc.)

• As soon as thermal testing is complete, we are ready As soon as thermal testing is complete, we are ready to begin production of the final system, complete with to begin production of the final system, complete with custom optics and electronics for processing of CCD custom optics and electronics for processing of CCD outputoutput

• We are currently building the final components of a We are currently building the final components of a prototype dewar for thermal testing prototype dewar for thermal testing

• We are already in possession of all the necessary We are already in possession of all the necessary equipment for thermal control of the system equipment for thermal control of the system (temperature controller, cooling system, vacuum (temperature controller, cooling system, vacuum fittings, etc.)fittings, etc.)

• As soon as thermal testing is complete, we are ready As soon as thermal testing is complete, we are ready to begin production of the final system, complete with to begin production of the final system, complete with custom optics and electronics for processing of CCD custom optics and electronics for processing of CCD outputoutput

71

Tightly coupled software/observingTightly coupled software/observingTightly coupled software/observingTightly coupled software/observing

Take Image 1Take Image 130 sec 30 sec

Analyze Image: Analyze Image: flatten, WCS, sextractor flatten, WCS, sextractor Galactic reddening corr.Galactic reddening corr.

Produce z, Produce z, zz

OK? OK?

OffsetOffsetTake Image 2Take Image 2

30 sec 30 sec

Slew to next targetSlew to next target

Offset if appropriateOffset if appropriate

More imagesMore images

72

Rapid Readout and High EfficiencyRapid Readout and High EfficiencyRapid Readout and High EfficiencyRapid Readout and High EfficiencyIntegrated SW reduces wasted timeIntegrated SW reduces wasted timeBinning 2x2 gives Binning 2x2 gives

• 0.124 arcsec/pix, • Single amplifier output per 2K x 4K chip

8 sec readout @ 250Kpix/sec

Effective telescope time multiplier:Effective telescope time multiplier:• For “balanced” exposures, sequential images take

Tseries = 4(texp+treadout)x Nframes • Parallel imager takes (with 0.8 throughput degradation)

Tparallel = (texp/0.8 + treadout) x Nframes

For texp>>treadout total time is reduced by a factor of ~3

Integrated SW reduces wasted timeIntegrated SW reduces wasted timeBinning 2x2 gives Binning 2x2 gives

• 0.124 arcsec/pix, • Single amplifier output per 2K x 4K chip

8 sec readout @ 250Kpix/sec

Effective telescope time multiplier:Effective telescope time multiplier:• For “balanced” exposures, sequential images take

Tseries = 4(texp+treadout)x Nframes • Parallel imager takes (with 0.8 throughput degradation)

Tparallel = (texp/0.8 + treadout) x Nframes

For texp>>treadout total time is reduced by a factor of ~3

73

Controlling SystematicsControlling SystematicsControlling SystematicsControlling Systematics

• Our design is readily baffledOur design is readily baffled• Can use both field stop and pupil stop• Suppresses stray and scattered light• Better flatfielding

• Single common shutter near pupilSingle common shutter near pupil• Reduced shutter artifacts

• Flux ratios with a single pointing and 2-3 Flux ratios with a single pointing and 2-3 exposures, under all conditions!exposures, under all conditions!

• Even with patchy cloud cover, get Poisson-limited colors.

• Our design is readily baffledOur design is readily baffled• Can use both field stop and pupil stop• Suppresses stray and scattered light• Better flatfielding

• Single common shutter near pupilSingle common shutter near pupil• Reduced shutter artifacts

• Flux ratios with a single pointing and 2-3 Flux ratios with a single pointing and 2-3 exposures, under all conditions!exposures, under all conditions!

• Even with patchy cloud cover, get Poisson-limited colors.

74

Complementarity Complementarity with Dark Energy Camerawith Dark Energy Camera

Complementarity Complementarity with Dark Energy Camerawith Dark Energy Camera

Multiband Camera:Multiband Camera: 16 arcmin 16 arcmin22, 6.5m aperture:, 6.5m aperture:

- Get 100 clusters to z~1 in 4 hours. - Get 100 clusters to z~1 in 4 hours.

- Can be on the sky at start of SPT survey- Can be on the sky at start of SPT survey

Dark Energy CameraDark Energy Camera: 3 sq deg, single band, 4m: 3 sq deg, single band, 4m aperture:aperture:

- Survey approach on CTIO 4m gets 3 sq deg x 7 clusters/sq deg = 21 - Survey approach on CTIO 4m gets 3 sq deg x 7 clusters/sq deg = 21 clusters per hour, or 84 clusters in 4 hours.clusters per hour, or 84 clusters in 4 hours.

- Delivers other science as well: weak lensing, SN detection... - Delivers other science as well: weak lensing, SN detection...

Multiband imager’s cluster hunting advantage is 100/84 = 1.2 Multiband imager’s cluster hunting advantage is 100/84 = 1.2 • Does not take into account seeing advantage on Magellan• Does not take into account cloud-immunity of multiband imager • If SPT survey falls short of flux goals, multiband advantage increases

Multiband camera better suited to chasing z>1 clusters. Multiband camera better suited to chasing z>1 clusters.

Multiband Camera:Multiband Camera: 16 arcmin 16 arcmin22, 6.5m aperture:, 6.5m aperture:

- Get 100 clusters to z~1 in 4 hours. - Get 100 clusters to z~1 in 4 hours.

- Can be on the sky at start of SPT survey- Can be on the sky at start of SPT survey

Dark Energy CameraDark Energy Camera: 3 sq deg, single band, 4m: 3 sq deg, single band, 4m aperture:aperture:

- Survey approach on CTIO 4m gets 3 sq deg x 7 clusters/sq deg = 21 - Survey approach on CTIO 4m gets 3 sq deg x 7 clusters/sq deg = 21 clusters per hour, or 84 clusters in 4 hours.clusters per hour, or 84 clusters in 4 hours.

- Delivers other science as well: weak lensing, SN detection... - Delivers other science as well: weak lensing, SN detection...

Multiband imager’s cluster hunting advantage is 100/84 = 1.2 Multiband imager’s cluster hunting advantage is 100/84 = 1.2 • Does not take into account seeing advantage on Magellan• Does not take into account cloud-immunity of multiband imager • If SPT survey falls short of flux goals, multiband advantage increases

Multiband camera better suited to chasing z>1 clusters. Multiband camera better suited to chasing z>1 clusters.

75

Two-stage planTwo-stage planTwo-stage planTwo-stage plan• 2007 – 20092007 – 2009: : SPT in operationSPT in operation Use multiband camera to image ~2000 clustersUse multiband camera to image ~2000 clusters

Initial cluster count vs. z resultsInitial cluster count vs. z results Use camera for SN followup as well...Use camera for SN followup as well...• Post-2009:Post-2009: Dark Energy Camera on Blanco 4m (if $)Dark Energy Camera on Blanco 4m (if $) Deep wide DEC survey will find SNe Deep wide DEC survey will find SNe Follow SN light curves with multiband cameraFollow SN light curves with multiband camera Chase higher-z clusters with multiband cameraChase higher-z clusters with multiband camera

• 2007 – 20092007 – 2009: : SPT in operationSPT in operation Use multiband camera to image ~2000 clustersUse multiband camera to image ~2000 clusters

Initial cluster count vs. z resultsInitial cluster count vs. z results Use camera for SN followup as well...Use camera for SN followup as well...• Post-2009:Post-2009: Dark Energy Camera on Blanco 4m (if $)Dark Energy Camera on Blanco 4m (if $) Deep wide DEC survey will find SNe Deep wide DEC survey will find SNe Follow SN light curves with multiband cameraFollow SN light curves with multiband camera Chase higher-z clusters with multiband cameraChase higher-z clusters with multiband camera

76

StatusStatusStatusStatus

• Conceptual design doneConceptual design done• Proof-of-concept optical design doneProof-of-concept optical design done• Detectors are in handDetectors are in hand

• Lincoln labs 2K x 4K, 15 m pixels• Some epitaxial, some high-resistivity

• Readout electronics require replicationReadout electronics require replication• MegaCam architecture and board set

• Thermal/cryo test dewar in fabricationThermal/cryo test dewar in fabrication

• Conceptual design doneConceptual design done• Proof-of-concept optical design doneProof-of-concept optical design done• Detectors are in handDetectors are in hand

• Lincoln labs 2K x 4K, 15 m pixels• Some epitaxial, some high-resistivity

• Readout electronics require replicationReadout electronics require replication• MegaCam architecture and board set

• Thermal/cryo test dewar in fabricationThermal/cryo test dewar in fabrication

77

Task listTask listTask listTask list• ModelingModeling

• Slew vs. expose tradeoffs vs. redshift and richness

• Photo-z determination

• HardwareHardware• Finish design work, order optics

• Mechanical design, fabrication

• Electronics and detector optimization

• System integration, testing...

• SoftwareSoftware• Scripts that connect Source Extractor to photoz codes

• Test with SDSS and IMACS data

• Integrate with instrument

• ModelingModeling• Slew vs. expose tradeoffs vs. redshift and richness

• Photo-z determination

• HardwareHardware• Finish design work, order optics

• Mechanical design, fabrication

• Electronics and detector optimization

• System integration, testing...

• SoftwareSoftware• Scripts that connect Source Extractor to photoz codes

• Test with SDSS and IMACS data

• Integrate with instrument

78

Multiband Camera SummaryMultiband Camera SummaryMultiband Camera SummaryMultiband Camera Summary• We have a unique opportunity:We have a unique opportunity:

• Multiple science drivers• Unique capability• Quality photometry

• Conceptual design completedConceptual design completed• Detectors on hand, optics straightforwardDetectors on hand, optics straightforward• Design needs to be refined, and optimal Design needs to be refined, and optimal

observing strategy devisedobserving strategy devised• Software is a key aspect. Software is a key aspect. • Important complement to other dark energy Important complement to other dark energy

measurementsmeasurements

• We have a unique opportunity:We have a unique opportunity:• Multiple science drivers• Unique capability• Quality photometry

• Conceptual design completedConceptual design completed• Detectors on hand, optics straightforwardDetectors on hand, optics straightforward• Design needs to be refined, and optimal Design needs to be refined, and optimal

observing strategy devisedobserving strategy devised• Software is a key aspect. Software is a key aspect. • Important complement to other dark energy Important complement to other dark energy

measurementsmeasurements

Final slideFinal slideFinal slideFinal slideLPPC is engaged in multiple cutting edge fundamental LPPC is engaged in multiple cutting edge fundamental astrophysics projects astrophysics projects

Main motivations are fundamental physics: Main motivations are fundamental physics:

Dark energy, dark matter. Dark energy, dark matter.

Technical infrastructure (electronics, machine shop, Technical infrastructure (electronics, machine shop, computing…) is essential to our successcomputing…) is essential to our success

Strong student interest in these topics: Strong student interest in these topics:

Grad students have opportunity to build and operate Grad students have opportunity to build and operate

apparatus within their PhD studiesapparatus within their PhD studies

Undergraduates will take part as well. Undergraduates will take part as well.

LPPC is engaged in multiple cutting edge fundamental LPPC is engaged in multiple cutting edge fundamental astrophysics projects astrophysics projects

Main motivations are fundamental physics: Main motivations are fundamental physics:

Dark energy, dark matter. Dark energy, dark matter.

Technical infrastructure (electronics, machine shop, Technical infrastructure (electronics, machine shop, computing…) is essential to our successcomputing…) is essential to our success

Strong student interest in these topics: Strong student interest in these topics:

Grad students have opportunity to build and operate Grad students have opportunity to build and operate

apparatus within their PhD studiesapparatus within their PhD studies

Undergraduates will take part as well. Undergraduates will take part as well.

80

Backup Slides and residual clutterBackup Slides and residual clutterBackup Slides and residual clutterBackup Slides and residual clutter

81

Cluster luminosity functionCluster luminosity functionCluster luminosity functionCluster luminosity function

DM= 38.2 implies L* ~ 17.1 AB r mag at z = 0.1DM= 38.2 implies L* ~ 17.1 AB r mag at z = 0.1DM= 38.2 implies L* ~ 17.1 AB r mag at z = 0.1DM= 38.2 implies L* ~ 17.1 AB r mag at z = 0.1

(M)(M)

Christlein and Zabludoff, astro-ph/0304031Christlein and Zabludoff, astro-ph/0304031

82

Solid: w= Solid: w= 11Dotted: w= Dotted: w= 0.60.6Shortdash: w= Shortdash: w= 0.20.2Longdash: open CDMLongdash: open CDM

83

Limiting MagnitudeLimiting Magnitude Limiting MagnitudeLimiting Magnitude

• ½ L* cluster galaxies at redshift ½ L* cluster galaxies at redshift 4000A break leaving blue filter4000A break leaving blue filter g,r,i,z = 22.8,23.4,24.0,23.3 Complete cluster catalog

• Galaxy catalog completenessGalaxy catalog completeness g,r,i,z = 22.8,23.4,24.0,23.6 Simple selection function

• Blue galaxy photo-z at faint magsBlue galaxy photo-z at faint mags g,r,i,z = 24.0,24.0,24.0,23.6 Photo-z for angular power spectra and

weak lensing

• ½ L* cluster galaxies at redshift ½ L* cluster galaxies at redshift 4000A break leaving blue filter4000A break leaving blue filter g,r,i,z = 22.8,23.4,24.0,23.3 Complete cluster catalog

• Galaxy catalog completenessGalaxy catalog completeness g,r,i,z = 22.8,23.4,24.0,23.6 Simple selection function

• Blue galaxy photo-z at faint magsBlue galaxy photo-z at faint mags g,r,i,z = 24.0,24.0,24.0,23.6 Photo-z for angular power spectra and

weak lensingA

B M

ag

o

f ½

L*

84

Next-Generation FacilitiesNext-Generation FacilitiesNext-Generation FacilitiesNext-Generation Facilities

Microwave background - Better angular resolution CMB mapsDetection of clusters of galaxies vs. z

Supernovae – Dedicated Dark Energy satellite missionLarge Synoptic Survey Telescope (LSST)

Weak Gravitational LensingBoth ground-based and space based

Probing the foundations of gravityEquivalence principleInverse square law

SNAP, Lawrence Berkeley LaboratorySNAP, Lawrence Berkeley Laboratory

LSST CorporationLSST Corporation

85

(Hubble Space Telescope, NASA)(Hubble Space Telescope, NASA)

Supernovae are powerful cosmological probes

Distances to ~6% from brightness

Redshifts from features in spectra

86

One One parameter parameter

family family

One One parameter parameter

family family

(Supernova Cosmology Project, Kim et al)

Color

Rate of decline

Peak brightness

~ 0.13 mag

87

Type Ia SNe are precise candlesType Ia SNe are precise candlesType Ia SNe are precise candlesType Ia SNe are precise candles

Jose Luis Prieto Krisciunas et al (2003)

σ~0.11mag

88

A Cosmic Sum RuleA Cosmic Sum RuleA Cosmic Sum RuleA Cosmic Sum Rule

General Relativity + isotropy and homogeneity require General Relativity + isotropy and homogeneity require that (in the relevant units)that (in the relevant units)

geometrygeometry + + mattermatter + + = 1 = 1

If the underlying geometry is flat, and if If the underlying geometry is flat, and if mm <1 then the <1 then the

cosmological constant term cosmological constant term must must be non-zero. be non-zero.

So it would seem……..So it would seem……..

89

High-z Supernova Search Team

Microwave Background

Cluster Masses

m

““Best Fit” at Best Fit” at

massmass ~ 0.3 ~ 0.3

~ 0.7~ 0.7

What does this mean?What does this mean?

Insufficient mass to halt the Insufficient mass to halt the expansionexpansion

Rate of expansion is Rate of expansion is increasing…increasing…

90

This picture is supported by multiple This picture is supported by multiple independent lines of evidenceindependent lines of evidence

This picture is supported by multiple This picture is supported by multiple independent lines of evidenceindependent lines of evidence

• Lower bound on age, from starsLower bound on age, from stars

• Inventories of cosmic matter contentInventories of cosmic matter content

• Measurements of expansion history using supernovaeMeasurements of expansion history using supernovae

• Primordial element abundances Primordial element abundances

• CMB provides strong confirmation…. WMAP CMB provides strong confirmation…. WMAP

• Lower bound on age, from starsLower bound on age, from stars

• Inventories of cosmic matter contentInventories of cosmic matter content

• Measurements of expansion history using supernovaeMeasurements of expansion history using supernovae

• Primordial element abundances Primordial element abundances

• CMB provides strong confirmation…. WMAP CMB provides strong confirmation…. WMAP

91

Redshift = Δ/

DistancetoSupernova

Faraway

Nearby0.01 0.1 1.0

Δ

Schmidt et al, High-z SN TeamSchmidt et al, High-z SN Team

92

Extinction by “gray” dust?Extinction by “gray” dust?Careful multicolor measurements, esp. in IRExploit different z-dependenceLook at SNe behind clusters of galaxies

““Evolutionary” Effects?Evolutionary” Effects?Use stellar populations of different ages as a proxy

Selection differences in nearby vs. distant Selection differences in nearby vs. distant samples?samples?

Increase the sample of well-monitored SneCalibrate detection efficiencies

K-corrections, Galactic extinction, K-corrections, Galactic extinction, photometric zeropoints....photometric zeropoints....

See See Leibundgut, astro-ph/0003326Leibundgut, astro-ph/0003326

Extinction by “gray” dust?Extinction by “gray” dust?Careful multicolor measurements, esp. in IRExploit different z-dependenceLook at SNe behind clusters of galaxies

““Evolutionary” Effects?Evolutionary” Effects?Use stellar populations of different ages as a proxy

Selection differences in nearby vs. distant Selection differences in nearby vs. distant samples?samples?

Increase the sample of well-monitored SneCalibrate detection efficiencies

K-corrections, Galactic extinction, K-corrections, Galactic extinction, photometric zeropoints....photometric zeropoints....

See See Leibundgut, astro-ph/0003326Leibundgut, astro-ph/0003326

93

WMAP- The Relic Hiss of WMAP- The Relic Hiss of the Big Bangthe Big Bang

WMAP- The Relic Hiss of WMAP- The Relic Hiss of the Big Bangthe Big Bang

                                                         

                             (NASA)(NASA)

94

Optical PerformanceOptical PerformanceOptical PerformanceOptical PerformancePlate scale is 0.062 arcsec per 15 Plate scale is 0.062 arcsec per 15 m pixelm pixel

FOV is 4.1 x 4.1 arcminutes (~ 700 kpc at z=0.3)FOV is 4.1 x 4.1 arcminutes (~ 700 kpc at z=0.3)

80% encircled energy in ~0.15 arcsec:80% encircled energy in ~0.15 arcsec:

Plate scale is 0.062 arcsec per 15 Plate scale is 0.062 arcsec per 15 m pixelm pixel

FOV is 4.1 x 4.1 arcminutes (~ 700 kpc at z=0.3)FOV is 4.1 x 4.1 arcminutes (~ 700 kpc at z=0.3)

80% encircled energy in ~0.15 arcsec:80% encircled energy in ~0.15 arcsec:

95

LSST Merges 3 Enabling LSST Merges 3 Enabling Technologies Technologies

LSST Merges 3 Enabling LSST Merges 3 Enabling Technologies Technologies

• Large Aperture OpticsLarge Aperture Optics

• Computing and Data Storage Computing and Data Storage

• High Efficiency DetectorsHigh Efficiency Detectors

• Large Aperture OpticsLarge Aperture Optics

• Computing and Data Storage Computing and Data Storage

• High Efficiency DetectorsHigh Efficiency Detectors

96

Large Mirror FabricationLarge Mirror FabricationLarge Mirror FabricationLarge Mirror Fabrication

University of ArizonaUniversity of Arizona

97

Cost per GigabyteCost per GigabyteCost per GigabyteCost per Gigabyte

98

Large Format CCD MosaicsLarge Format CCD MosaicsLarge Format CCD MosaicsLarge Format CCD MosaicsMegacam, CfA/HarvardMegacam, CfA/Harvard