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Update on LSST & GSMT Jeremy Mould

Users Committee October 13, 2004

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GSMT SWG

The GSMT SWG is a community-based group convened to:

• Formulate a powerful science case for federal investment in GSMT

– Identify key science drivers

– Develop clear and compelling arguments for GSMT in the era of JWST/ALMA

– Discuss realization of key science as a function of design parameters: aperture,

FOV, PSF……

• Generate unified, coherent community support

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GSMT SWG Members

Chair: Rolf-Peter Kudritzki, UH IfA

SWG Members:

– Jill Bechtold -- UA– Mike Bolte -- UCSC– Ray Carlberg -- U of T– Matthew Colless -- ANU– Irena Cruz-Gonzales -- UNAM– Alan Dressler -- OCIW– Betsy Gillespie -- UA

–Terry Herter -- Cornell

–Jonathan Lunine -- UA LPL

–Claire Max -- UCSC

–Chris McKee -- UCB

–Francois Rigaut -- Gemini

–Chuck Steidel -- CIT

–Steve Strom -- NOAO

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TMT is a fusion of 3 concepts

The GSMT, CELT and VLOT point design telescope concepts.

GSMT CELT VLOT

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TMT Project FY2004

• Project Office established• Project manager appointed• Engineering efforts from 4 partners integrated to provide a 'reference

design'    – based on the heritage of the VLOT, CELT and GSMT efforts

• Moore funds in place for D and D Phase (gift to UC & Caltech)• CFI funds authorized• NSF proposal submitted• Key milestone: Baseline Design which will answer the following key design

issues/trades– Is the elevation axis in front of or behind the primary? – Is the telescope optical configuration RC or AG?– What is the focal ratio of the primary ( f/1 – f/1.5)? – What final focal ratios should be provided ( f/15 – f/22)?

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Highest Priority Capabilities for First Light

• diffraction-limited (10 mas @ 1.6) imaging & spectroscopy– 0.8- to 2.5-micron wavelength– 1-2 arcminutes multi-conjugate adaptive optics (MCAO) field– Strehl ratio at K-band of 0.7, constant across the field to 10%;– highly-multiplexed (~1,000 slits)

• seeing-limited 100 < R < 7,000 spectroscopy – 0.32- to 1-micron wavelength range– wide (10-20 arc-minute) field

• high-spectral-resolution (20,000 < R < 100,000) spectroscopy – 1- to 5-micron– 7- to 28-micron

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TMT phased implementation

• optical spectroscopy with 20,000 < R < 100,000 – 0.3 microns to 1 micron

• very high-contrast imaging near diffraction limit 1 to 2.5– contrast ratio > 108 at> 4/D from bright stars

• R ~3,000-5,000 spectroscopy – fields ≥5 arcminutes – 0.7- to 2.5-micron – sampling 0.15 arcseconds– image quality 80% enclosed energy in 0.3 arc-sec. – unit (IFU) heads or microslits – ground-layer adaptive optics system (GLAO);

• mid-IR diffraction-limited imaging (Strehl > 0.5, 7 < < 28) over a field >30 arcseconds;

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TMT AO modes

AO mode Enables ScienceMid-IR NGS AO Diffraction limited

resolution > MPlanet-forming Environments

MCAO Diffraction-limited resolution in J, H, K bands over 0.5-1’ fields

Galaxy Assembly; deconstructing stellar populations

MOAO ~0.1” resolution over 3-5’ fields for multi-object spectroscopy

Young galaxy mass, metallicity, & star formation

ExAO High dynamic range imaging

Planet detection & characterization

GLAO 0.2-3” resolution over 5-10’ fields

Galaxy evolution

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NIO

• provided 'point design' for GSMT -- key element of TMT planning

• supports site testing (northern chile; Baja, CA; Hawaii); serves both theGMT and TMT communities

• interfaces with ESO to advance technologies of mutual interest

• has contributed key technical and management leadership within TMT

• post TMT project office, NIO will– carry out two key  TMT work packages (mid-IR Echelle; M2 assembly)– continue site testing– continue ESO collaborations (level TBD following allocation of TMT workpackages)

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GSMT vs JWST

Simulated monochromatic images of the ‘Antennae’ (local starburst galaxy: 105 seconds integration time)Courtesy: Elizabeth Barton, GSMT SWG

JWSTGSMT

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GMT alternate

Giant Magellan Telescope (GMT)

7 x 8.4 meter mirrors

Magellan partners + Texas

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OIR Planning

• Long Range Planning Committee (Chair: C. Pilachowski) is currently working on a roadmap for large scale facilities http://www.noao.edu/dir/lrplan/lrp-committee.html

• Where will the decision points be for public funding ?• Look forward from 2005 as far as 2030.

– Two decadal surveys will occur before 2025, and these will outrank this roadmap.

• The plan will show how present investments – realize the new initiatives, – illustrate convergence paths, – lay the basis for facility closures and transfers, – and address community structural change.

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Overview and Status

Opportunities for Scientific Participation

9 October 2004

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LSST Partners

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Project Technical Status

Systems Engineering – Requirements and Scope

~3 GigapixelCamera

8.4m 3-mirror8.4m 3-mirrorTelescopeTelescope Data Products &Data Products &

ManagementManagement

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Observing Simulator

• Initially Created By Abi Saha

• New Simulation Tool in Development– K. Cook et. al.– Foundation and

Testbed for Scheduler

A. Saha, NOAO

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• Nature of Dark Energy– Image Quality – FWHM <0.8arcsec– Shape Systematics – PSF (e1,e2) < 0.0001

• Solar System Map– Observing Cadence– Absolute Astrometry – Link Vectors From Multiple Epochs

• Optical Transients – Observing Cadence– Data Processing – Real-Time Alerts (~30sec delay)

• Galactic Structure– Photometric Precision – 1% Internal, 2% Absolute– Astrometry

The LSST Key Science Drivers

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Mapping the Solar System: Probing the Fossil Record

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Mapping the Galactic Halo

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Weak Lensing and Cosmology

• Cluster tomography– Shear used to obtain mass maps– Number density of clusters as function of redshift depends

on density fluctuations and distance scale– Both depend on dark energy

• Strauss report– Power spectrum, bispectrum, and shear cosmography

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Special cadence to go deeper?

23T3=3.25, CC2=-0.5501

Evolving Optical Design

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Wide – Deep - Fast

• ~10 deg.2 per Field• ~7m Effective Collecting Area• m~24th per 10 sec Exposure• Wide Coverage > 15,000 Square Degrees• Multiple Filters (e.g. bgriz´ - TBD)• ~100+ Epochs in Each of >1500 Fields in Each Filter

Over Ten Years• Accumulated Depth of 26th Magnitude in Each Filter

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Schedule & Milestones

2004 20102005 2006 2007 2008 2009 2011 2012 2013

Design

Construction

Integration

Commissioning

Operation

First Light

CoDR PDR CDR

Optics on site

First Light

Order glass Start finalcamera fab

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Camera

• Focal Plane Array– 10 m pixels 0.2 arcsecond/pixel (~1/3 seeing-limited PSF)

– 64 cm diameter 10 square degree FOV

3 Gpixels– Integrated front-end electronics– 16 bits/pixel, 2 sec readout time 3 GB/sec

Parallel readout

• Housing / Filters / Optics / Mechanisms

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• Private Donor Committed to Buy LSST Mirror– University of Arizona Borosilicate Cast Mirror

– Similar to LBT Primary with Very Large Hole

• Contract Approved – Materials and Engineering

– Casting

– Optical Figuring

– Cell Integration and Testing

Primary Mirror Contract

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Telescope Structure

• Initial Warren Davidson Study Complete– Long Tube

– Stiff Structure, f(n1)=10hz

– Relatively Light , 200T

• Preparing for Second Study– Short Tube– Open Structure– Industrial Source

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Site Selection

• First Down-Selection Completed in May 2004• Cerro Pachon • Las Campanas • San Pedro Martir • La Palma

• Study to Evaluate Satellite Data Issues • Correlating Local Data to Global Weather Patterns • Final Site (2) Selection Meeting 14 January 2005

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Summary

• LSST Corporation is Established• The Mission is Solidifying• Management Organized & Vision is Clear• Project Teams Developing• Technical Advancement Accelerating