1. GSMT Committee, Los Angeles, Oct. 20, 2005 1 Giant Magellan Telescope

2. GSMT Committee, Los Angeles, Oct. 20, 2005 2 GSMT Committee Requests Baseline Design First & Second Generation AO Capabilities Project Schedule & Milestones First-Light & Second Generation Instruments Operations Models Public Access

3. GSMT Committee, Los Angeles, Oct. 20, 2005 3 GMT Partners Carnegie Institution of Washington Harvard University Massachusetts Institute of Technology University of Arizona University of Michigan Smithsonian Institution The University of Texas at Austin Texas A&M University

4. GSMT Committee, Los Angeles, Oct. 20, 2005 4 Telescope Structure & Optics

5. GSMT Committee, Los Angeles, Oct. 20, 2005 5 GMT Optical Design Primary Mirror D1 = 25.4 meter R1 = 36.0 meters K = -0.9983 f/0.7 primary mirror overall Gregorian secondary mirror D2 = 3.2 meter R2 = 4.2 meter K2 = -0.7109 1.06 m Segments aligned with primary mirrors Combined Aplanatic Gregorian focus f/8.2 final focal ratio Field of view: ~20-24 arc-min. BFD = 5.5 meters M2 conjugate = 160 m above M1

6. GSMT Committee, Los Angeles, Oct. 20, 2005 6 GMT Studies Structure FEA static and modal analysis Dynamic response to wind disturbance Optics handling & exchange Mechanisms Hydrostatic bearings Drives Instrument rotator platform Mirror covers Manufacturability & Cost

7. GSMT Committee, Los Angeles, Oct. 20, 2005 7 Primary Mirror GMT1 Objectives Develop the technology for casting and polishing 8.4-m off-axis aspheric mirrors. Casting & generating non-symmetric blanks Metrology for testing highly aspheric off-axis mirrors Polishing with stressed lap Establish the pipeline for sequential processing of mirrors. Schedule requires ~1 finished mirror per year after ramp-up. Production of the first GMT primary mirror segment. Status of GMT1 fabrication-- On Schedule Blank is cast Projected furnace opening October 24 Preparations underway for lifting and clean-out of the blank Modifications of test tower underway

8. GSMT Committee, Los Angeles, Oct. 20, 2005 8 SOML Casting & Cleanout Areas

9. GSMT Committee, Los Angeles, Oct. 20, 2005 9 Primary Mirror Off-axis Prototype

10. GSMT Committee, Los Angeles, Oct. 20, 2005 10 GMT1 Casting- 7/23/05 Peak T = 1160  C Currently T ~ 20  C

11. GSMT Committee, Los Angeles, Oct. 20, 2005 11 Steward Observatory Mirror Lab LPM LOGTest tower Stressed lap

12. GSMT Committee, Los Angeles, Oct. 20, 2005 12 Load-spreader Layout Quads Singles Doubles Triples

13. GSMT Committee, Los Angeles, Oct. 20, 2005 13 Triple Support Actuator Triple actuator Loadspreader Mirror Cell top plate

14. GSMT Committee, Los Angeles, Oct. 20, 2005 14 Predicted Performance Horizon pointing Specification: Ro=150 cm. Baseline actuator types are not ganged. Zenith pointing (no gravity sags). Specification: Ro= 214 cm.

15. GSMT Committee, Los Angeles, Oct. 20, 2005 15 Adaptive Optics Development AO modes Extreme (high-contrast, high SR, single object) AO (ExAO) Ground Layer (wide-field) AO (GLAO) Laser Tomography (all-sky, high Strehl-ratio, narrow field) AO (LTAO) AO system components AO secondary mirror Laser guide star system Optical Switch yard AO wavefront sensors Wavefront reconstructor(s)

16. GSMT Committee, Los Angeles, Oct. 20, 2005 16 Secondary Mirror

17. GSMT Committee, Los Angeles, Oct. 20, 2005 17 Laser Projection Laser House Beam Projector Na Laser beams (6)

18. GSMT Committee, Los Angeles, Oct. 20, 2005 18 AO Optical Switchyard

19. GSMT Committee, Los Angeles, Oct. 20, 2005 19 Magellan (Manqui)Campanas Pk. Alcaino Pk. Ridge (Manquis) LCO Sites

20. GSMT Committee, Los Angeles, Oct. 20, 2005 20 North West Manquis (100”) Manqui (Magellan) Alcaino (Nagoya) Las Campanas La Mollaca Alta Seeing Towers & weather stations: 5 km NE Wind (80%) SW Wind (20%) 2308 2450 2410 2551 2726

21. GSMT Committee, Los Angeles, Oct. 20, 2005 21 Site Testing Table 1. Status at the LCO test sites SiteLocationElevation (m) Status 2Saddle near duPont Telescope2308 1.DIMM operating 2.Weather station operating 3Manqui: Next to Clay Telescope 2450 1.MASS/DIMM operating. 2.Weather station operating 4Las Campanas Peak2551 1.DIMM is operating. 2.Weather station operating. 5Alcaino Peak: Ex-Nagoya2410 1.DIMM is operating. 2.Weather station operating. 3.PWV monitors

22. GSMT Committee, Los Angeles, Oct. 20, 2005 22 DIMM Results from 4 Sites

23. GSMT Committee, Los Angeles, Oct. 20, 2005 23 Baseline Site Campanas PK.

24. GSMT Committee, Los Angeles, Oct. 20, 2005 24 GMT Site Layout from E

25. GSMT Committee, Los Angeles, Oct. 20, 2005 25 GMT viewed from SW

26. GSMT Committee, Los Angeles, Oct. 20, 2005 26 GMT (top view from N)

27. GSMT Committee, Los Angeles, Oct. 20, 2005 27 Conceptual Design Review Topics Science Case & Technical Requirements Operations plan Design & Feasibility studies for telescope & enclosure subsystems Cost & schedule projections Implementation plan Date: February 21-23 Location: Pasadena CA

28. GSMT Committee, Los Angeles, Oct. 20, 2005 28

29. GSMT Committee, Los Angeles, Oct. 20, 2005 29 GMT Science Working Group

30. GSMT Committee, Los Angeles, Oct. 20, 2005 30 GMT Science Working Group Warrick Couch Australia Xiaohui Fan Arizona Karl Gebhardt Texas Gary Hill Texas John Huchra Harvard Scott Kenyon Smithsonian Pat McCarthy Carnegie Michael Meyer Arizona Alycia Weinberger Carnegie/DTM

31. GSMT Committee, Los Angeles, Oct. 20, 2005 31 GMT SWG Reports GMT for Dummies - GMT for Dummies - Science Case V 1.0 - 3.4 Science Case V 1.0 - 3.4 GMT Overview - GMT Overview - Science Requirements Document V 2.4 Science Requirements Document V 2.4 Site Selection Report V 3.4 Site Selection Report V 3.4 Joint Opportunities with GMT & ALMA V 2.0 Joint Opportunities with GMT & ALMA V 2.0 Operations Model V 1.0 Operations Model V 1.0 Science Case V 4.1 Science Case V 4.1

32. GSMT Committee, Los Angeles, Oct. 20, 2005 32 GMT Science Requirements 1. High Level Science Goals 2. Definition of the Telescope and Related Facilities 3. Site Requirements 4. First Generation Instrument Specifications 5. Adaptive Optics Capabilities 6. Support Facilities 7. Operational Requirements 8. Image Size and Wave-Front Requirements

33. GSMT Committee, Los Angeles, Oct. 20, 2005 33 HighLevelScienceGoals

34. GSMT Committee, Los Angeles, Oct. 20, 2005 34 GMT Instruments InstrumentP.I.ModePort 1. Visible-band Multi-object Spectrograph S. ShectmanNatural seeing, GLAOGregorian 2. High Resolution Visible Spectrograph P. McQueenNatural seeingFolded Port 3. Near-IR Multi-Object Spectrograph D. FabricantNatural Seeing, GLAOGregorian 4. Near-IR Extreme AO Imager L. CloseExAOFolded Port 5. Near-IR High Resolution Spectrometers D. JaffeNatural seeing, LTAOFolded port 6. Mid-IR AO Imager & Spectrograph P. HinzLTAOFolded port

35. GSMT Committee, Los Angeles, Oct. 20, 2005 35 Instrument Match to Science Goals

36. GSMT Committee, Los Angeles, Oct. 20, 2005 36 First Generation Instrument Candidates 1. Visible Multi-Object Spectrograph Four-Arm Double Spectrograph 18’ x 9’ FOV - VPH grisms - Transmission optics R ~ 3500 (red) & ~ 1200 (blue) primary mode higher and low R modes available Multiplexing factor ~ 500 - 1000 depending on mode

37. GSMT Committee, Los Angeles, Oct. 20, 2005 37 GMACS- Visible band MOS Shectman, et. al.

38. GSMT Committee, Los Angeles, Oct. 20, 2005 38 GMACS- Visible band MOS

39. GSMT Committee, Los Angeles, Oct. 20, 2005 39 First Generation Instrument Candidates 3. Near-IR Multi-Object Spectrograph Refractive Optics - Collimator-Camera Design 7’ x 7’ Imaging Field - 5’ x 7’ Spectroscopic R = 3200 & R = 1500 modes 10k x 6k detector mosaic  (80) < 0.15” - 0.067” pixels IFU mode under development

40. GSMT Committee, Los Angeles, Oct. 20, 2005 40 GMT NIRMOS Instrument Mounting Flange Support Roller Interface Ring Fabricant, et. al.

41. GSMT Committee, Los Angeles, Oct. 20, 2005 41 GMT NIRMOS Instrument Platform Available Cassegrain Instrument Volume 6.35 m 5.2 m 7.62 m

42. GSMT Committee, Los Angeles, Oct. 20, 2005 42 First Generation Instrument Candidates 5. High Resolution Near-IR Spectrograph Two Channels: 1 - 2.5  m Natural Seeing or AO 3 - 5  m Diffraction-Limited Silicon Immersion gratings R ~ 25-100k (JHK) & 100-150K (L&M) 4k x 4k HgCdTe FPAs

43. GSMT Committee, Los Angeles, Oct. 20, 2005 43 Near-IR High-resolution Spectrometer Short wavelength module: J, K, H Jaffe, et. al.

44. GSMT Committee, Los Angeles, Oct. 20, 2005 44 GMT Instrument Platform (IP) Rotator GLAO Guider Folded port instruments Gregorian instruments capacity 6.4 m Dia. 7.6 m high 25 ton

45. GSMT Committee, Los Angeles, Oct. 20, 2005 45 First Generation Instruments Fibre-based spectrographs: Bragg Fibre OH suppression, massive multiplexing Narrow-band imaging tuneable filters Deployable IFUs diffraction-limit and coarse scales (GLAO?) Second-Pass Instrument Development

46. GSMT Committee, Los Angeles, Oct. 20, 2005 46 Adaptive Optics Goals 1.Extreme AO exoplanets, debris disks 2. Ground-Layer Correction faint galaxies, stellar populations, surveys 3. Laser Tomography morphological studies, dynamics First Generation AO Capabilities

47. GSMT Committee, Los Angeles, Oct. 20, 2005 47 Adaptive Optics Goals Second Generation AO Capabilities 1.Multi-Conjugate AO Stellar populations, Galactic taxonomy 2. Multi-Object AO faint galaxies, Stellar populations, Dynamics

48. GSMT Committee, Los Angeles, Oct. 20, 2005 48 Operation Principles Maximize Scientific Output of Facility - Maximize Flexibility to Changing Conditions & Opportunities - Maximize Operating Efficiency Minimize Operating Costs

49. GSMT Committee, Los Angeles, Oct. 20, 2005 49 Operating Modes Classical PI Mode Queue Service Observing Target of Opportunity and Synoptic Observing Campaign Mode

50. GSMT Committee, Los Angeles, Oct. 20, 2005 50 Operations Model “Flexible Assisted Observing” Base Schedule in Blocks of PI, Queue & Campaign Time Shared Nights Preemption of Base Schedule in Response to Weather, Synoptic and TOO Feed-Back loop for Tracking and Balancing Partner Time

51. GSMT Committee, Los Angeles, Oct. 20, 2005 51 Staffing Implications “Flexible Assisted Observing” Telescope Operators Resident Astronomers Instrument Operators & Specialists AO & Laser Support Team

52. GSMT Committee, Los Angeles, Oct. 20, 2005 52 Operations Cost Staffing Level: 114 FTEs (~ 30 US, ~84 Chile) Instrumentation: 2 Instruments under contract at any time, new capital instrument every 3-4 years. Facility upgrades: Allow for improvements in telescope, coating chambers, etc. Administrative Costs: Corporate officers, insurance etc.

53. GSMT Committee, Los Angeles, Oct. 20, 2005 53 Operations vs. Capital Our Model for GMT Operations: ~ 6% of Capital Magellan: 5% Keck: ~ 7% VLT: ~ 8% Gemini: 18%

54. GSMT Committee, Los Angeles, Oct. 20, 2005 54 Community Access AURA-led joint proposal to NSF for Technology Development ensures access to broad US community in proportion to public investment AURA, NOAO, NSF have observer status on GMT Board GMT partnership agreement defines modes by which access can be obtained: capital contributions instrumentation development operations support Broader community input to design and development is envisioned

55. GSMT Committee, Los Angeles, Oct. 20, 2005 55

56. GSMT Committee, Los Angeles, Oct. 20, 2005 56 Model B (Hex Truss) - Mode 7, 8.00 Hz

57. GSMT Committee, Los Angeles, Oct. 20, 2005 57 Model A: Original – Braced Hexapod Brackets Model B: Upper Hexapod Truss Model C: 2x Wall Thickness Vent gates open Pointing Error RMS Y Direction (arcsec) Original Upper Hex Truss Upper Hex 2x Wall Thickness Minimum0.3800.2520.303 Maximum0.4010.2680.321 Average0.3920.2610.313 Combined0.3850.2560.308 Wind 13 m/s, vents open

58. GSMT Committee, Los Angeles, Oct. 20, 2005 58 Model B (Hex Truss) - Mode 7, 8.00 Hz