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

2. 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. 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. 4 TMT is a fusion of 3 concepts The GSMT, CELT and VLOT point design telescope concepts. GSMT CELT VLOT

5. 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. 6 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

7. 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 2.5  –contrast ratio > 10 8 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  30 arcseconds;

8. 8 TMT AO modes AO modeEnablesScience Mid-IR NGS AODiffraction limited resolution > M Planet-forming Environments MCAODiffraction-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 ExAOHigh dynamic range imaging Planet detection & characterization GLAO0.2-3” resolution over 5- 10’ fields Galaxy evolution

9. 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. 10 GSMT vs JWST Simulated monochromatic images of the ‘Antennae’ (local starburst galaxy: 10 5 seconds integration time) Courtesy: Elizabeth Barton, GSMT SWG JWST GSMT

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

12. 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. 13 Overview and Status Opportunities for Scientific Participation 9 October 2004

14. 14 LSST Partners

15. 15 Project Technical Status Systems Engineering – Requirements and Scope ~3 Gigapixel Camera 8.4m 3-mirror Telescope Data Products & Management

16. 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. 17 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

18. 18

19. 19 Mapping the Solar System: Probing the Fossil Record

20. 20 Mapping the Galactic Halo

21. 21 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

22. 22 Special cadence to go deeper?

23. 23 T3=3.25, CC2=-0.5501 Evolving Optical Design

24. 24

25. 25 Wide – Deep - Fast ~10 deg. 2 per Field ~7m Effective Collecting Area m~24 th 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 26 th Magnitude in Each Filter

26. 26 Schedule & Milestones 2004201020052006200720082009201120122013 Design Construction Integration Commissioning Operation First Light CoDR PDRCDR Optics on site First Light Order glass Start final camera fab

27. 27 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

28. 28 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

29. 29 Telescope Structure Initial Warren Davidson Study Complete –Long Tube –Stiff Structure, f(n 1 )=10hz –Relatively Light, 200T Preparing for Second Study –Short Tube –Open Structure –Industrial Source

30. 30 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

31. 31 Summary LSST Corporation is Established The Mission is Solidifying Management Organized & Vision is Clear Project Teams Developing Technical Advancement Accelerating