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

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

GSMT Committee, Los Angeles, Oct. 20, GMT Optical Design Primary Mirror D1 = 25.4 meter R1 = 36.0 meters K = f/0.7 primary mirror overall Gregorian secondary mirror D2 = 3.2 meter R2 = 4.2 meter K2 = 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, 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, 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, SOML Casting & Cleanout Areas

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

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

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

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

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

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

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

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

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

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

GSMT Committee, Los Angeles, Oct. 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%)

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

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

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

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

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

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

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

GSMT Committee, Los Angeles, Oct. 20,

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

GSMT Committee, Los Angeles, Oct. 20, 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

GSMT Committee, Los Angeles, Oct. 20, GMT SWG Reports GMT for Dummies - GMT for Dummies - Science Case V Science Case V 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

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

GSMT Committee, Los Angeles, Oct. 20, 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

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

GSMT Committee, Los Angeles, Oct. 20, 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 ~ depending on mode

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

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

GSMT Committee, Los Angeles, Oct. 20, 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” ” pixels IFU mode under development

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

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

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

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

GSMT Committee, Los Angeles, Oct. 20, 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, 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

GSMT Committee, Los Angeles, Oct. 20, 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

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

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

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

GSMT Committee, Los Angeles, Oct. 20, 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,

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

GSMT Committee, Los Angeles, Oct. 20, 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 Minimum Maximum Average Combined Wind 13 m/s, vents open

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