Giant Magellan Telescope

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Giant Magellan Telescope
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GSMT Committee Requests

• Baseline Design
• First Second Generation AO Capabilities
• Project Schedule Milestones
• First-Light Second Generation Instruments
• Operations Models
• Public Access

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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 AM University

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Telescope Structure Optics
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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

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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

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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

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SOML Casting Cleanout Areas
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Primary Mirror Off-axis Prototype
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GMT1 Casting- 7/23/05
Peak T 1160? C Currently T 20? C
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Steward Observatory Mirror Lab
LOG
Test tower
LPM
Stressed lap
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Load-spreader Layout
Doubles
Quads
Singles
Triples
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Triple Support Actuator
Mirror
Loadspreader
Cell top plate
Triple actuator
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Predicted Performance
Horizon pointing Specification Ro150 cm.
Baseline actuator types are not ganged.
Zenith pointing (no gravity sags). Specification
Ro 214 cm.
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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)

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Secondary Mirror
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Laser Projection
Beam Projector
Na Laser beams (6)
Laser House
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AO Optical Switchyard
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LCO Sites
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North
Manquis (100)
Manqui (Magellan)
NE Wind (80)
Alcaino (Nagoya)
2308
2450
La Mollaca Alta
2410
5 km
West
Las Campanas
2726
2551
SW Wind (20)
Seeing Towers weather stations
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Site Testing
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DIMM Results from 4 Sites
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Baseline Site
Campanas PK.
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GMT Site Layout from E
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GMT viewed from SW
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GMT (top view from N)
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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

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GMT Science Working Group
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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

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GMT SWG Reports

• GMT for Dummies
  -
• Science Case
  V 1.0 - 3.4
• GMT Overview
  -
• 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

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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
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High Level Science Goals
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GMT Instruments
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Instrument Match to Science Goals
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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
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GMACS- Visible band MOS
Shectman, et. al.
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GMACS- Visible band MOS
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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) lt 0.15 - 0.067 pixels
IFU mode under development
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GMT NIRMOS
Fabricant, et. al.
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GMT NIRMOS
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First Generation Instrument Candidates
5. High Resolution Near-IR Spectrograph
Two Channels 1 - 2.5mm Natural Seeing or
AO 3 - 5mm
Diffraction-Limited Silicon Immersion
gratings R 25-100k (JHK) 100-150K
(LM) 4k x 4k HgCdTe FPAs
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Near-IR High-resolution Spectrometer
Short wavelength module J, K, H
Jaffe, et. al.
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GMT Instrument Platform (IP)
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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?)

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Adaptive Optics Goals
First Generation AO Capabilities

• Extreme AO
• exoplanets, debris disks
• 2. Ground-Layer Correction
• faint galaxies, stellar populations,
  surveys
• 3. Laser Tomography
• morphological studies, dynamics

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Adaptive Optics Goals
Second Generation AO Capabilities

• Multi-Conjugate AO
• Stellar populations, Galactic taxonomy
• 2. Multi-Object AO
• faint galaxies, Stellar populations,
  Dynamics

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Operation Principles

• Maximize Scientific Output of Facility
• - Maximize Flexibility to Changing
  Conditions Opportunities
• - Maximize Operating Efficiency
• Minimize Operating Costs

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Operating Modes

• Classical PI Mode
• Queue Service Observing
• Target of Opportunity and Synoptic Observing
• Campaign Mode

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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

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Staffing Implications

• Flexible Assisted Observing
• Telescope Operators
• Resident Astronomers
• Instrument Operators Specialists
• AO Laser Support Team

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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.

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Operations vs. Capital

• Our Model for GMT Operations 6 of
  Capital
• Magellan
  5
• Keck
  7
• VLT
  8
• Gemini
  18

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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

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Model B (Hex Truss) - Mode 7, 8.00 Hz
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Model A Original Braced Hexapod Brackets
Model B Upper Hexapod Truss
Model C 2x Wall Thickness
Wind 13 m/s, vents open
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Model B (Hex Truss) - Mode 7, 8.00 Hz