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Update on LSST & GSMT Jeremy Mould Users Committee October 13, 2004 1 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 2 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 3 TMT is a fusion of 3 concepts GSMT CELT VLOT The GSMT, CELT and VLOT point design telescope concepts. 4 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)? 5 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 6 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 < l < 28m) over a field >30 arcseconds; 7 TMT AO modes AO mode Enables Science Mid-IR NGS AO Diffraction limited resolution l > M Planet-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 35’ 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- Galaxy evolution 10’ fields 8 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) 9 GSMT vs JWST Simulated monochromatic images of the ‘Antennae’ (local starburst galaxy: 105 seconds integration time) Courtesy: Elizabeth Barton, GSMT SWG GSMT JWST 10 GMT alternate Magellan partners + Texas 7 x 8.4 meter mirrors Giant Magellan Telescope (GMT) 11 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. 12 Overview and Status Opportunities for Scientific Participation 9 October 2004 13 LSST Partners 14 Project Technical Status Systems Engineering – Requirements and Scope ~3 Gigapixel Camera 8.4m 3-mirror Telescope Data Products & Management 15 Observing Simulator • Initially Created By Abi Saha • New Simulation Tool in Development – K. Cook et. al. – Foundation and Testbed for Scheduler A. Saha, NOAO 16 The LSST Key Science Drivers • Nature of Dark Energy – – • Solar System Map – – • Observing Cadence Absolute Astrometry – Link Vectors From Multiple Epochs Optical Transients – – • Image Quality – FWHM <0.8arcsec Shape Systematics – PSF (e1,e2) < 0.0001 Observing Cadence Data Processing – Real-Time Alerts (~30sec delay) Galactic Structure – – Photometric Precision – 1% Internal, 2% Absolute Astrometry 17 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 Generator Enclosure (separate) 28 m D (92') dome 800 s.f. Mechanical Equipment (interior) Mechanical Equipment (exterior) 650 s.f. 750 s.f. Observing Level 49'-0" (15 m) Data Processing Room Utility Level 33'-0" Machine Shop Camera Iinstrument Shop 3200 s.f. 640 s.f. 860 s.f. Receiving 820 s.f. Base Level 0'-0" W.C. 70 s.f. Break Room 190 s.f. W.C. 70 s.f. Control Room 650 s.f. Enclosure & Platform Lift Section office 130 s.f. office 130 s.f. coating chamber mirror prep area office 130 s.f. Work Stations (~8 people) 640 s.f. office 130 s.f. shop storage Summit Support Facility Plan platform lift 0 0 v. elex 6' 7' Base Level Enclosure Plan 5 10 30 ft. 5 10 m J. Barr 12 Aug, '04 LSST Facilities Conceptual Layout 24 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 25 Schedule & Milestones First Light 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 CoDR PDR CDR Design Order glass Construction Start final camera fab Optics on site Integration First Light Commissioning Operation 26 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 27 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 28 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 29 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 30 Summary • • • • • LSST Corporation is Established The Mission is Solidifying Management Organized & Vision is Clear Project Teams Developing Technical Advancement Accelerating 31