GSMT Committee, Los Angeles, Oct. 20, 2005 1

Giant Magellan Telescope

GSMT Committee, Los Angeles, Oct. 20, 2005 2

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 3

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 4

Telescope Structure & Optics

GSMT Committee, Los Angeles, Oct. 20, 2005 5

GMT Optical DesignPrimary Mirror

D1 = 25.4 meter

R1 = 36.0 meters

K = -0.9983

f/0.7 primary mirror overall

Gregorian secondary mirrorD2 = 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 metersM2 conjugate = 160 m above M1

GSMT Committee, Los Angeles, Oct. 20, 2005 6

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 7

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 8

SOML Casting & Cleanout Areas

GSMT Committee, Los Angeles, Oct. 20, 2005 9

Primary Mirror Off-axis Prototype

GSMT Committee, Los Angeles, Oct. 20, 2005 10

GMT1 Casting- 7/23/05

Peak T = 1160 C

Currently T ~ 20 C

GSMT Committee, Los Angeles, Oct. 20, 2005 11

Steward Observatory Mirror Lab

LPM

LOGTest tower

Stressed lap

GSMT Committee, Los Angeles, Oct. 20, 2005 12

Load-spreader Layout

Quads

Singles

Doubles

Triples

GSMT Committee, Los Angeles, Oct. 20, 2005 13

Triple Support Actuator

Triple actuator

Loadspreader

Mirror

Cell top plate

GSMT Committee, Los Angeles, Oct. 20, 2005 14

Predicted PerformanceZenith to Horizon Performance

0.0

50.0

100.0

150.0

200.0

250.0

300.0

350.0

0.00 2.00 4.00 6.00 8.00 10.00Distance, m

WF height diff, nm-rms

Allowable,Ro=150 cmLBT typeactuatorsGangedPressures

Zenith Pointing Performance

0.0

50.0

100.0

150.0

200.0

250.0

0.00 1.00 2.00 3.00 4.00 5.00 6.00 7.00 8.00 9.00Distance, m

WF height diff., nm-rms

Allowable,Ro=214 cm

LBT type

GangedPressures

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 15

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 16

Secondary Mirror

GSMT Committee, Los Angeles, Oct. 20, 2005 17

Laser Projection

Laser House

Beam Projector

Na Laser beams (6)

GSMT Committee, Los Angeles, Oct. 20, 2005 18

AO Optical Switchyard

GSMT Committee, Los Angeles, Oct. 20, 2005 19

Magellan (Manqui) Campanas Pk.

Alcaino Pk.

Ridge (Manquis)

LCO Sites

GSMT Committee, Los Angeles, Oct. 20, 2005 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%)

2308

2450

2410

2551

2726

GSMT Committee, Los Angeles, Oct. 20, 2005 21

Site TestingTable 1. Status at the LCO test sites

Site Location Elevation(m)

Status

2 Saddle near duPont Telescope 23081. DIMM operating2. Weather station operating

3 Manqui: Next to Clay Telescope

24501. MASS/DIMM operating.2. Weather station operating

4 Las Campanas Peak 25511. DIMM is operating.2. Weather station operating.

5 Alcaino Peak: Ex-Nagoya 24101. DIMM is operating.2. Weather station operating.3. PWV monitors

GSMT Committee, Los Angeles, Oct. 20, 2005 22

DIMM Results from 4 Sites

GSMT Committee, Los Angeles, Oct. 20, 2005 23

Baseline Site

Campanas PK.

GSMT Committee, Los Angeles, Oct. 20, 2005 24

GMT Site Layout from E

GSMT Committee, Los Angeles, Oct. 20, 2005 25

GMT viewed from SW

GSMT Committee, Los Angeles, Oct. 20, 2005 26

GMT (top view from N)

GSMT Committee, Los Angeles, Oct. 20, 2005 27

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 28

GSMT Committee, Los Angeles, Oct. 20, 2005 29

GMT Science Working GroupGMT Science Working Group

GSMT Committee, Los Angeles, Oct. 20, 2005 30

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 31

GMT SWG Reports

• GMT for Dummies - GMT for Dummies -

• Science Case V 1.0 - 3.4Science Case V 1.0 - 3.4

• GMT Overview -GMT Overview -

• Science Requirements Document V 2.4Science Requirements Document V 2.4

• Site Selection Report V 3.4Site Selection Report V 3.4

• Joint Opportunities with GMT & ALMA V 2.0Joint Opportunities with GMT & ALMA V 2.0

• Operations Model V 1.0Operations Model V 1.0

• Science Case V 4.1Science Case V 4.1

GSMT Committee, Los Angeles, Oct. 20, 2005 32

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 33

High High

LevelLevel

SciencScience e

GoalsGoals

GSMT Committee, Los Angeles, Oct. 20, 2005 34

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

4. Near-IR Extreme AO Imager

L. Close ExAO Folded Port

5. Near-IR High Resolution Spectrometers

D. Jaffe Natural seeing, LTAO Folded port

6. Mid-IR AO Imager & Spectrograph

P. Hinz LTAO Folded port

GSMT Committee, Los Angeles, Oct. 20, 2005 35

Instrument Match to Science Goals# Science Area Sub-Area Instruments Notes1 Exoplanets Direct imaging 6, 4 ExAO, Nulling

Disks scattering 6, 4Disk emission 4, 6 mid-IRRadial vel. surveys 3, 5

2 Solar System KBOs 1, 6Comets & Moons 3, 5, 4

3 Star Formation Embedded clusters 6, 4Proper motions 1 GLAO criticalCrowded fields 6, 2, 1Mass ratios 6, 3, 5

4 Stellar Pops Stellar abundances 3, 5Pop. Studies 1, 6, 3

5 Black Holes AGN Environments 1, 6, 2 IFU,TF ModesVelocity structures 6, 1 IFU Mode

6 Dark Energy SNe monitoring 6, 1, 2SNe physics 1, 2 Polarim. mode

7 Galaxy Ass. Stellar mass density 1, 2Internal dynamics 2, 6

8 First Light IGM studies 1, 3, 2, 5First Galaxies 1, 2, 6

GSMT Committee, Los Angeles, Oct. 20, 2005 36

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 37

GMACS- Visible band MOS

Shectman, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005 38

GMACS- Visible band MOS

GSMT Committee, Los Angeles, Oct. 20, 2005 39

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” - 0.067” pixels

IFU mode under development

GSMT Committee, Los Angeles, Oct. 20, 2005 40

GMT NIRMOSInstrument Mounting

Flange

Support Roller Interface Ring

Fabricant, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005 41

GMT NIRMOS

Instrument Platform

Available Cassegrain Instrument Volume

6.35 m

5.2 m

7.62 m

GSMT Committee, Los Angeles, Oct. 20, 2005 42

First Generation Instrument Candidates

5. High Resolution Near-IR Spectrograph

Two Channels: 1 - 2.5m Natural Seeing or AO

3 - 5m 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 43

Near-IR High-resolution Spectrometer

Short wavelength module: J, K, H

Jaffe, et. al.

GSMT Committee, Los Angeles, Oct. 20, 2005 44

GMT Instrument Platform (IP)

RotatorGLAO Guider

Folded portinstruments

Gregorianinstruments

capacity6.4 m Dia.7.6 m high

25 ton

GSMT Committee, Los Angeles, Oct. 20, 2005 45

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 DevelopmentSecond-Pass Instrument Development

GSMT Committee, Los Angeles, Oct. 20, 2005 46

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 CapabilitiesFirst Generation AO Capabilities

GSMT Committee, Los Angeles, Oct. 20, 2005 47

Adaptive Optics Goals

Second Generation AO CapabilitiesSecond 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 48

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 49

Operating Modes

• Classical PI Mode

• Queue Service Observing

• Target of Opportunity and Synoptic Observing

• Campaign Mode

GSMT Committee, Los Angeles, Oct. 20, 2005 50

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 51

Staffing Implications

“Flexible Assisted Observing”

• Telescope Operators

• Resident Astronomers

• Instrument Operators & Specialists

• AO & Laser Support Team

GSMT Committee, Los Angeles, Oct. 20, 2005 52

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 53

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 54

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 55

GSMT Committee, Los Angeles, Oct. 20, 2005 56

Model B (Hex Truss) - Mode 7, 8.00 Hz

QuickTime™ and aCinepak decompressor

are needed to see this picture.

GSMT Committee, Los Angeles, Oct. 20, 2005 57

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

1.E-03

1.E-02

1.E-01

1.E+00

0.1 1 10 100

Frequency (Hz)

Mirror 7

Mirror 1

Mirror 2

Mirror 3

Mirror 4

Mirror 5

Mirror 6

Combined Mirrors

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

1.E-03

1.E-02

1.E-01

1.E+00

0.1 1 10 100

Frequency (Hz)

1.E-08

1.E-07

1.E-06

1.E-05

1.E-04

1.E-03

1.E-02

1.E-01

1.E+00

0.1 1 10 100

Frequency (Hz)

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)

  OriginalUpper Hex

Truss

Upper Hex 2x Wall

Thickness

Minimum 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

Wind 13 m/s, vents open

GSMT Committee, Los Angeles, Oct. 20, 2005 58

Model B (Hex Truss) - Mode 7, 8.00 Hz