Download GMT - AURA

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
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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
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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
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Triple Support Actuator
Mirror
Loadspreader
Cell top plate
Triple actuator
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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Secondary Mirror
GSMT Committee, Los Angeles, Oct. 20, 2005
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Laser Projection
Beam Projector
Na Laser beams
(6)
Laser House
GSMT Committee, Los Angeles, Oct. 20, 2005
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AO Optical Switchyard
GSMT Committee, Los Angeles, Oct. 20, 2005
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LCO Sites
Magellan (Manqui)
Campanas Pk.
Alcaino Pk.
Ridge (Manquis)
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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DIMM Results from 4 Sites
GSMT Committee, Los Angeles, Oct. 20, 2005
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Baseline Site
Campanas PK.
GSMT Committee, Los Angeles, Oct. 20, 2005
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GMT Site Layout from E
GSMT Committee, Los Angeles, Oct. 20, 2005
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GMT viewed from SW
GSMT Committee, Los Angeles, Oct. 20, 2005
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GMT (top view from N)
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
GSMT Committee, Los Angeles, Oct. 20, 2005
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GSMT Committee, Los Angeles, Oct. 20, 2005
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GMT Science Working Group
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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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
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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
GSMT Committee, Los Angeles, Oct. 20, 2005
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High
Level
Science
Goals
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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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
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GMACS- Visible band MOS
Shectman, et. al.
GSMT Committee, Los Angeles, Oct. 20, 2005
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GMACS- Visible band MOS
GSMT Committee, Los Angeles, Oct. 20, 2005
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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) < 0.15” - 0.067” pixels
IFU mode under development
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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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
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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
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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?)
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
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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
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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
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Operating Modes
• Classical PI Mode
• Queue Service Observing
• Target of Opportunity and Synoptic Observing
• Campaign Mode
GSMT Committee, Los Angeles, Oct. 20, 2005
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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
GSMT Committee, Los Angeles, Oct. 20, 2005
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Staffing Implications
“Flexible Assisted Observing”
• Telescope Operators
• Resident Astronomers
• Instrument Operators & Specialists
• AO & Laser Support Team
GSMT Committee, Los Angeles, Oct. 20, 2005
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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.
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
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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