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Giant Magellan Telescope. GSMT Committee Requests. Baseline Design First & Second Generation AO Capabilities Project Schedule & Milestones First-Light & Second Generation Instruments Operations Models Public Access. GMT Partners. Carnegie Institution of Washington Harvard University

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giant magellan telescope
Giant Magellan Telescope

GSMT Committee, Los Angeles, Oct. 20, 2005

gsmt committee requests
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

gmt partners
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

telescope structure optics
Telescope Structure & Optics

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt optical design
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

gmt studies
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

primary mirror gmt1
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

soml casting cleanout areas
SOML Casting & Cleanout Areas

GSMT Committee, Los Angeles, Oct. 20, 2005

primary mirror off axis prototype
Primary Mirror Off-axis Prototype

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt1 casting 7 23 05
GMT1 Casting- 7/23/05

Peak T = 1160 C

Currently T ~ 20 C

GSMT Committee, Los Angeles, Oct. 20, 2005

steward observatory mirror lab
Steward Observatory Mirror Lab

Test tower

LOG

LPM

Stressed lap

GSMT Committee, Los Angeles, Oct. 20, 2005

load spreader layout
Load-spreader Layout

Doubles

Quads

Singles

Triples

GSMT Committee, Los Angeles, Oct. 20, 2005

triple support actuator
Triple Support Actuator

Mirror

Loadspreader

Cell top plate

Triple actuator

GSMT Committee, Los Angeles, Oct. 20, 2005

predicted performance
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, 2005

adaptive optics development
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

secondary mirror
Secondary Mirror

GSMT Committee, Los Angeles, Oct. 20, 2005

laser projection
Laser Projection

Beam Projector

Na Laser beams (6)

Laser House

GSMT Committee, Los Angeles, Oct. 20, 2005

ao optical switchyard
AO Optical Switchyard

GSMT Committee, Los Angeles, Oct. 20, 2005

lco sites

Magellan (Manqui)

Campanas Pk.

Alcaino Pk.

Ridge (Manquis)

LCO Sites

GSMT Committee, Los Angeles, Oct. 20, 2005

slide20

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

site testing
Site Testing

GSMT Committee, Los Angeles, Oct. 20, 2005

dimm results from 4 sites
DIMM Results from 4 Sites

GSMT Committee, Los Angeles, Oct. 20, 2005

baseline site
Baseline Site

Campanas PK.

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt site layout from e
GMT Site Layout from E

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt viewed from sw
GMT viewed from SW

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt top view from n
GMT (top view from N)

GSMT Committee, Los Angeles, Oct. 20, 2005

conceptual design review
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

slide29

GMT Science Working Group

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt science working group
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, 2005

gmt swg reports
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

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt science requirements
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

slide33

High

Level

Science

Goals

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt instruments
GMT Instruments

GSMT Committee, Los Angeles, Oct. 20, 2005

instrument match to science goals
Instrument Match to Science Goals

GSMT Committee, Los Angeles, Oct. 20, 2005

first generation instrument candidates
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

gmacs visible band mos
GMACS- Visible band MOS

Shectman, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005

gmacs visible band mos38
GMACS- Visible band MOS

GSMT Committee, Los Angeles, Oct. 20, 2005

first generation instrument candidates39
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

gmt nirmos

Instrument Mounting

Flange

Support Roller Interface Ring

GMT NIRMOS

Fabricant, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt nirmos41

Instrument Platform

5.2 m

7.62 m

Available Cassegrain

Instrument Volume

6.35 m

GMT NIRMOS

GSMT Committee, Los Angeles, Oct. 20, 2005

first generation instrument candidates42
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 (L&M)

4k x 4k HgCdTe FPAs

GSMT Committee, Los Angeles, Oct. 20, 2005

near ir high resolution spectrometer
Near-IR High-resolution Spectrometer

Short wavelength module: J, K, H

Jaffe, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005

gmt instrument platform ip

Rotator

GLAO Guider

Folded port

instruments

Gregorian

instruments

capacity

6.4 m Dia.

7.6 m high

25 ton

GMT Instrument Platform (IP)

GSMT Committee, Los Angeles, Oct. 20, 2005

first generation instruments
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

adaptive optics goals
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

GSMT Committee, Los Angeles, Oct. 20, 2005

adaptive optics goals47
Adaptive Optics Goals

Second Generation AO Capabilities

Multi-Conjugate AO

Stellar populations, Galactic taxonomy

2. Multi-Object AO

faint galaxies, Stellar populations, Dynamics

GSMT Committee, Los Angeles, Oct. 20, 2005

operation principles
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

operating modes
Operating Modes
  • Classical PI Mode
  • Queue Service Observing
  • Target of Opportunity and Synoptic Observing
  • Campaign Mode

GSMT Committee, Los Angeles, Oct. 20, 2005

operations model
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

staffing implications
Staffing Implications

“Flexible Assisted Observing”

  • Telescope Operators
  • Resident Astronomers
  • Instrument Operators & Specialists
  • AO & Laser Support Team

GSMT Committee, Los Angeles, Oct. 20, 2005

operations cost
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

operations vs capital
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, 2005

community access
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

model b hex truss mode 7 8 00 hz
Model B (Hex Truss) - Mode 7, 8.00 Hz

GSMT Committee, Los Angeles, Oct. 20, 2005

slide57

Model A:

Original – Braced Hexapod Brackets

Model B:

Upper Hexapod Truss

Model C:

2x Wall Thickness

Wind 13 m/s, vents open

GSMT Committee, Los Angeles, Oct. 20, 2005

model b hex truss mode 7 8 00 hz58
Model B (Hex Truss) - Mode 7, 8.00 Hz

GSMT Committee, Los Angeles, Oct. 20, 2005