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Update on LSST & GSMT

This update provides information on the GSMT SWG, GSMT, CELT, VLOT, TMT Project, TMT phased implementation, TMT AO modes, NIO, JWST, GMT, OIR planning, and LSST.

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Update on LSST & GSMT

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  1. Update on LSST & GSMT Jeremy Mould Users Committee October 13, 2004

  2. 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

  3. 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

  4. GSMT CELT VLOT The GSMT, CELT and VLOT point design telescope concepts. TMT is a fusion of 3 concepts

  5. 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)?

  6. Highest Priority Capabilities for First Light • diffraction-limited (10 mas @ 1.6m) 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

  7. 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 2.5m • contrast ratio > 108 at q > 4l/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, 7m <  < 28m) over a field >30 arcseconds;

  8. TMT AO modes

  9. 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)

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

  11. Giant Magellan Telescope (GMT) GMT alternate Magellan partners + Texas 7 x 8.4 meter mirrors

  12. 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.

  13. Overview and StatusOpportunities for Scientific Participation 9 October 2004

  14. LSST Partners

  15. 8.4m 3-mirrorTelescope ~3 GigapixelCamera Data Products &Management Project Technical Status Systems Engineering – Requirements and Scope

  16. Observing Simulator • Initially Created By Abi Saha • New Simulation Tool in Development • K. Cook et. al. • Foundation and Testbed for Scheduler A. Saha, NOAO

  17. The LSST Key Science Drivers • 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

  18. Mapping the Solar System: Probing the Fossil Record

  19. Mapping the Galactic Halo

  20. 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

  21. Special cadence to go deeper?

  22. Evolving Optical Design T3=3.25, CC2=-0.5501

  23. 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

  24. First Light 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 CoDR PDR CDR Design Order glass Optics on site Construction Start final camerafab First Light Integration Commissioning Operation Schedule & Milestones

  25. Camera • Focal Plane Array • 10 mm 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

  26. Primary Mirror Contract • 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

  27. 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

  28. 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

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

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