Update on LSST & GSMT
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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?
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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