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Giant Magellan Telescope GSMT Committee, Los Angeles, Oct. 20, 2005 1 GSMT Committee Requests • Baseline Design • First & Second Generation AO Capabilities • Project Schedule & Milestones • First-Light & Second Generation Instruments • Operations Models • Public Access GSMT Committee, Los Angeles, Oct. 20, 2005 2 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 GSMT Committee, Los Angeles, Oct. 20, 2005 3 Telescope Structure & Optics GSMT Committee, Los Angeles, Oct. 20, 2005 4 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 GSMT Committee, Los Angeles, Oct. 20, 2005 5 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 GSMT Committee, Los Angeles, Oct. 20, 2005 6 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 GSMT Committee, Los Angeles, Oct. 20, 2005 7 SOML Casting & Cleanout Areas GSMT Committee, Los Angeles, Oct. 20, 2005 8 Primary Mirror Off-axis Prototype GSMT Committee, Los Angeles, Oct. 20, 2005 9 GMT1 Casting- 7/23/05 Peak T = 1160 C Currently T ~ 20 C GSMT Committee, Los Angeles, Oct. 20, 2005 10 Steward Observatory Mirror Lab Test tower LOG LPM Stressed lap GSMT Committee, Los Angeles, Oct. 20, 2005 11 Load-spreader Layout Doubles Quads Singles Triples GSMT Committee, Los Angeles, Oct. 20, 2005 12 Triple Support Actuator Mirror Loadspreader Cell top plate Triple actuator GSMT Committee, Los Angeles, Oct. 20, 2005 13 Predicted Performance Zenith to Horizon Performance Allowable, Ro=150 cm LBT type actuators Ganged Pressures 350.0 WF height diff, nm-rms 300.0 250.0 200.0 Horizon pointing Specification: Ro=150 cm. 150.0 100.0 Baseline actuator types are not ganged. 50.0 0.0 0.00 2.00 4.00 6.00 8.00 10.00 Distance, m Zenith Pointing Performance Zenith pointing 250.0 (no gravity sags). WF height diff., nm-rms 200.0 Allowable, Ro=214 cm LBT type 150.0 Specification: Ro= 214 cm. Ganged Pressures 100.0 50.0 0.0 0.00 1.00 2.00 Committee, 3.00 4.00 Los 5.00 Angeles, 6.00 7.00 8.00 2005 9.00 GSMT Oct. 20, Distance, m 14 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) GSMT Committee, Los Angeles, Oct. 20, 2005 15 Secondary Mirror GSMT Committee, Los Angeles, Oct. 20, 2005 16 Laser Projection Beam Projector Na Laser beams (6) Laser House GSMT Committee, Los Angeles, Oct. 20, 2005 17 AO Optical Switchyard GSMT Committee, Los Angeles, Oct. 20, 2005 18 LCO Sites Magellan (Manqui) Campanas Pk. Alcaino Pk. Ridge (Manquis) GSMT Committee, Los Angeles, Oct. 20, 2005 19 North Manquis (100”) Manqui (Magellan) NE Wind (80%) 2308 Alcaino (Nagoya) 2450 La Mollaca Alta 2410 5 km West Las Campanas 2726 2551 SW Wind (20%) Seeing Towers & weather stations: GSMT Committee, Los Angeles, Oct. 20, 2005 20 Site Testing Table 1. Status at the LCO test sites Site Location Elevation (m) 2 Saddle near duPont Telescope 2308 Status 1. DIMM operating 2. Weather station operating 3 4 Manqui: Next to Clay Telescope 2450 Las Campanas Peak 2551 1. MASS/DIMM operating. 2. Weather station operating 1. 2. 5 Alcaino Peak: Ex-Nagoya DIMM is operating. Weather station operating. 2410 1. DIMM is operating. 2. Weather station operating. 3. PWV monitors GSMT Committee, Los Angeles, Oct. 20, 2005 21 DIMM Results from 4 Sites GSMT Committee, Los Angeles, Oct. 20, 2005 22 Baseline Site Campanas PK. GSMT Committee, Los Angeles, Oct. 20, 2005 23 GMT Site Layout from E GSMT Committee, Los Angeles, Oct. 20, 2005 24 GMT viewed from SW GSMT Committee, Los Angeles, Oct. 20, 2005 25 GMT (top view from N) GSMT Committee, Los Angeles, Oct. 20, 2005 26 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 GSMT Committee, Los Angeles, Oct. 20, 2005 27 GSMT Committee, Los Angeles, Oct. 20, 2005 28 GMT Science Working Group GSMT Committee, Los Angeles, Oct. 20, 2005 29 GMT Science Working Group • Warrick Couch • Scott Kenyon Australia Smithsonian • Xiaohui Fan • Pat McCarthy Arizona Carnegie • Karl Gebhardt • Michael Meyer Texas • Gary Hill Arizona • Alycia Weinberger Texas Carnegie/DTM • John Huchra Harvard GSMT Committee, Los Angeles, Oct. 20, 2005 30 GMT SWG Reports • GMT for Dummies • Science Case • GMT Overview V 1.0 - 3.4 - • Science Requirements Document V 2.4 • Site Selection Report V 3.4 • Joint Opportunities with GMT & ALMA V 2.0 • Operations Model V 1.0 • Science Case V 4.1 GSMT Committee, Los Angeles, Oct. 20, 2005 31 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 GSMT Committee, Los Angeles, Oct. 20, 2005 32 High Level Science Goals GSMT Committee, Los Angeles, Oct. 20, 2005 33 GMT Instruments Instrument P.I. Mode Port 1. Visible-band Multi-object Spectrograph S. Shectman Natural seeing, GLAO Gregorian 2. High Resolution Visible Spectrograph P. McQueen Natural seeing Folded Port 3. Near-IR Multi-Object Spectrograph D. Fabricant Natural Seeing, GLAO Gregorian L. Close ExAO Folded Port 5. Near-IR High Resolution Spectrometers D. Jaffe Natural seeing, LTAO Folded port 6. P. Hinz LTAO Folded port 4. Near-IR Extreme AO Imager Mid-IR AO Imager & Spectrograph GSMT Committee, Los Angeles, Oct. 20, 2005 34 Instrument Match to Science Goals # 1 Science Area Exopl anets 2 Solar System 3 Star Formation 4 Stell ar Pops 5 Black Holes 6 Dark Energy 7 Galaxy Ass. 8 First Li ght Sub-Area Dir ect im aging Disks scattering Disk emission Radial ve l. survey s KBOs Comets & Moons Embedded clusters Proper motion s Crowded fie lds Mass ratios Stell ar abundan ces Pop. Studi es AGN Env ir onments Velocit y structures SNe moni toring SNe phys ics Stell ar mass dens it y Internal dyna mi cs IGM studies First Galaxies GSMT Committee, Los Angeles, Oct. 20, 2005 Instruments 6, 4 6, 4 4, 6 3, 5 1, 6 3, 5, 4 6, 4 1 6, 2, 1 6, 3, 5 3, 5 1, 6, 3 1, 6, 2 6, 1 6, 1, 2 1, 2 1, 2 2, 6 1, 3, 2, 5 1, 2, 6 Notes ExAO, Nulli ng mi d-IR GLAO criti cal IFU,TF Modes IFU Mode Polarim. m ode 35 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 GSMT Committee, Los Angeles, Oct. 20, 2005 36 GMACS- Visible band MOS Shectman, et. al. GSMT Committee, Los Angeles, Oct. 20, 2005 37 GMACS- Visible band MOS GSMT Committee, Los Angeles, Oct. 20, 2005 38 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 q(80) < 0.15” - 0.067” pixels IFU mode under development GSMT Committee, Los Angeles, Oct. 20, 2005 39 GMT NIRMOS Instrument Mounting Flange Support Roller Interface Ring GSMT Committee, Los Angeles, Oct. 20, 2005 Fabricant, et. al. 40 GMT NIRMOS Instrument Platform 5.2 m 7.62 m Available Cassegrain Instrument Volume 6.35 m GSMT Committee, Los Angeles, Oct. 20, 2005 41 First Generation Instrument Candidates 5. High Resolution Near-IR Spectrograph Two Channels: 1 - 2.5mm 3 - 5mm Natural Seeing or AO Diffraction-Limited Silicon Immersion gratings R ~ 25-100k (JHK) & 100-150K (L&M) 4k x 4k HgCdTe FPAs GSMT Committee, Los Angeles, Oct. 20, 2005 42 Near-IR High-resolution Spectrometer Short wavelength module: J, K, H tertiary FPA primary secondary cross disperser echelle fold slit collimator Jaffe, et. al. GSMT Committee, Los Angeles, Oct. 20, 2005 200.00 mm Scale: 1/8 43 GMT Instrument Platform (IP) Rotator GLAO Guider Folded port instruments Gregorian instruments capacity 6.4 m Dia. 7.6 m high 25 ton GSMT Committee, Los Angeles, Oct. 20, 2005 44 First Generation Instruments Second-Pass Instrument Development • Fibre-based spectrographs: Bragg Fibre OH suppression, massive multiplexing • Narrow-band imaging tuneable filters • Deployable IFUs diffraction-limit and coarse scales (GLAO?) GSMT Committee, Los Angeles, Oct. 20, 2005 45 Adaptive Optics Goals First Generation AO Capabilities 1. Extreme AO exoplanets, debris disks 2. Ground-Layer Correction faint galaxies, stellar populations, surveys 3. Laser Tomography morphological studies, dynamics GSMT Committee, Los Angeles, Oct. 20, 2005 46 Adaptive Optics Goals Second Generation AO Capabilities 1. Multi-Conjugate AO Stellar populations, Galactic taxonomy 2. Multi-Object AO faint galaxies, Stellar populations, Dynamics GSMT Committee, Los Angeles, Oct. 20, 2005 47 Operation Principles • Maximize Scientific Output of Facility - Maximize Flexibility to Changing Conditions & Opportunities - Maximize Operating Efficiency • Minimize Operating Costs GSMT Committee, Los Angeles, Oct. 20, 2005 48 Operating Modes • Classical PI Mode • Queue Service Observing • Target of Opportunity and Synoptic Observing • Campaign Mode GSMT Committee, Los Angeles, Oct. 20, 2005 49 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 GSMT Committee, Los Angeles, Oct. 20, 2005 50 Staffing Implications “Flexible Assisted Observing” • Telescope Operators • Resident Astronomers • Instrument Operators & Specialists • AO & Laser Support Team GSMT Committee, Los Angeles, Oct. 20, 2005 51 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. GSMT Committee, Los Angeles, Oct. 20, 2005 52 Operations vs. Capital Our Model for GMT Operations: Magellan: Keck: ~ 6% of Capital 5% ~ 7% VLT: ~ 8% Gemini: 18% GSMT Committee, Los Angeles, Oct. 20, 2005 53 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 GSMT Committee, Los Angeles, Oct. 20, 2005 54 GSMT Committee, Los Angeles, Oct. 20, 2005 55 Model B (Hex Truss) - Mode 7, 8.00 Hz QuickTime™ and a Cinepak decompressor are needed to see this picture. GSMT Committee, Los Angeles, Oct. 20, 2005 56 Pointing Error, Y Direction 1.E+00 1.E+00 1.E-01 1.E-01 1.E-02 1.E-02 Pointing Error (arc sec^2/Hz) Pointing Error (arc sec^2/Hz) Pointing Error, Y Direction 1.E-03 1.E-04 1.E-05 Mirror 7 Mirror 1 Mirror 2 Mirror 3 Mirror 4 Mirror 5 Mirror 6 Combined Mirrors Mirror 7 1.E-03 Mirror 1 Mirror 2 Mirror 3 1.E-04 Mirror 4 Mirror 5 Mirror 6 1.E-05 Combined Mirrors 1.E-06 1.E-06 Model A: Original – Braced Hexapod Brackets 1.E-07 Model B: Upper Hexapod Truss 1.E-07 1.E-08 1.E-08 0.1 1 10 Pointing Error, Y Direction 100 0.1 1 10 100 Frequency (Hz) Frequency (Hz) 1.E+00 Vent gates open 1.E-01 Pointing Error RMS Pointing Error (arc sec^2/Hz) 1.E-02 Y Direction (arcsec) Mirror 7 Mirror 1 Mirror 2 Mirror 3 Mirror 4 Mirror 5 Mirror 6 Minimum Combined Mirrors 1.E-03 1.E-04 1.E-05 1.E-06 Model C: 2x Wall Thickness 1.E-07 Original Upper Hex Truss Upper Hex 2x Wall Thickness 0.380 0.252 0.303 Maximum 0.401 0.268 0.321 Average 0.392 0.261 0.313 Combined 0.385 0.256 0.308 1.E-08 0.1 1 10 Frequency (Hz) 100 GSMT Committee, Los Angeles, Oct. 20, 2005 Wind 13 m/s, vents open 57 Model B (Hex Truss) - Mode 7, 8.00 Hz GSMT Committee, Los Angeles, Oct. 20, 2005 58