Giant Magellan Telescope Project...

GMT Project Status, March 2011 1

Giant Magellan Telescope

Project Status

Patrick McCarthyDirector - GMTO

GMT Project Status, March 2011

Topics

• Partnership, Funding, Staffing, Organization• Science Case Review• Technical Status

• Schedule• Telescope• Primary Mirrors• Adaptive Optics• Site

• Things to Think About During the Week

GMT Institutions

HarvardCarnegie

Texas A&M

KASI U. Arizona

U. Texas Austin

Chicago!

GMT Partnership and Funding

AALANUArizonaCarnegieChicagoHarvardKASISmithsonianTexas A&MTexas Austin

Full FundingAALANUCarnegieKASI

PartialOther FoundersUS NSF

GMT Org Chart

All of the group lead positions are now

filled

Astro-2010

Decadal Survey Report

“New Worlds” - Exoplanets

“New Horizons” - First light & Reionization

Astro-2010

Decadal Survey Report

18/20 Key science goals addressed by GMT

4/5 Discovery areas opened by GMT

Updating the Science Case

Update of the Science Case is underway

Exoplanets TinneyStar and Planet Formation WeinbergerStellar Populations FrebelGalaxy Evolution & Black Holes PapovichFirst Light & Reionization FinkelsteinDark Matter, Energy GladdersTime-Domain Chen

First Drafts – mostly doneComment period via open Wiki – soon!

The GMT Concept

Giant-Segmented Mirror Telescope

Increased angular resolution:

10 mas at 1µm with AOover ~30’’ field of view

0.2” FWHM over~5 arc-minutes with GLAO

Increased collecting Area:

380 square meters

10 x Magellan 6.5m Telescope

The GMT Concept

380 square meters

The GMT Concept

380 square meters

New Horizons - The First GalaxiesObservationTheory

~ few photons per hour with Hubble

~ several photons per minute with GMT!10

First Light and Reionization

VLT & SINFONI14 hours

Lehnert et al. NATUREGMT & GMTNIFS

14 hours

Steve Finkelstein – TAMU

Resolved Stellar Populations

Factor of 3 improvement in image size is huge in confused regions

Gemini 8m

GMT 25m

Project Schedule

Near Term

• We are midway through the design phase

• Design progressing, some prototyping, primary mirror development

• Preconstruction site work

• Subsystems reviews in 2012, PDR in Fall 2012

Longer Term

• Primary mirrors remain pacing item

• Construction of major systems should start in 2013, site construction ~ 2014

• Commissioning start 2019

• Science operations 2020, shared risk observing in 2019

Telescope Structure

Seismic analysis• Modal Analysis using GMT FSM• Damping 0.5%, 2.0%, 5.0%• Operation level earthquake = 200 yr. return• Survival level earthquake = 500 yr. return• Input conditions typical of Andes foothills• Soil conditions similar to Magellan = hard rock• Assumes primary mirror on static supports

Design accelerations (2% damping)Design accelerations (2% damping)Design accelerations (2% damping)

Location OLE SLE

Ground level .28g .34g

Instrument Platform 1.1g 1.4g

Primary mirror 3.5g 4.5g

Secondary mirror 4.1g 5.3g

Primary Mirror Supports & Ventilator Assemblies

Ventilators (~50) (blue) Hardpoints (6)

(magenta)

Triple-axis actuators (85)

(brown)Single-axis

actuators (80) (red & green)

Cell top plate (gray)

Actuators

Actuator assembly

Mirror

Loadspreader Assy Cell top plate

Triple-axis Actuator

Gimble attachment to cell

Mirror interface

Motorized jack-screw assembly

Force break-away mechanism

Load cell

HardpointDesigns nearing completion – prototyping next

First Off-Axis GMT Primary Segment

Primary Polishing

Stressed Lap ”Silly Putty” Lap

Metrology- 3 tests

Alignment of the Test Optics

GMT1 Surface as of mid Feb

First Off-Axis GMT Primary Segment

Second Segment Casting planned for December

AO System Performance

SJ = 36%

SH = 56%

SK = 72%

SL’ = 90%SM = 94%

On-axis total wave-front error: 196nm

Wavelength (µm)

Adaptive Secondary Mirror (ASM)

Fixed Flange

Hexapod

Electronics

Mobile Flange

Cold plate

2 mm Face sheet & magnets (not shown)

Reference body & electromagnets

The Large Binocular

Telescope ASM

Viewed from below, with face sheet removed

Viewed from above

LBT GMT

Diameter 94 cm 101 cm

Actuators 672 672

The LBT PSF in detail

Challenges for the GMT, Melbourne, June 16 2010 2727

Linear intensity scale

Seeing = 0.7”

Log intensity scale

Seeing = 0.7”

Log intensity scale

mv = 5.8

Seeing = 0.7”

Log intensity scale

4 s exposure

mv = 5.8

Seeing = 0.7”

Log intensity scale

4 s exposure

mv = 5.8

SR = 68%

LBT Adaptive Secondary

HST WFC3 LBT with AO~15”

Adaptive Secondary Mirror (ASM)

Hexapod

Interface

Telescope structure

Controller

Wind shield

DM assembly• Cold plate• Reference Body• Face sheet

First round of design studies and cost estimate

complete

Las Campanas Observatory

Alcaino Pk. (2410 m)

Manqui Pk. (2450 m)

(Magellan 6.5m telescopes)

Campanas Pk. (2551 m)

Manquis Ridge (2308 m)

(DuPont 100” telescope)

Pan American Hwy (Route 5)

Seeing Statistics 2005-2008

Seeing Percen*les 10% 25% 50% 75% 90%

Manquis Ridge 0.46 0.55 0.67 0.85 1.07

Co. Manqui 0.42 0.51 0.62 0.79 0.99

Co. Alcaino 0.42 0.50 0.62 0.79 1.01

Co. Las Campanas 0.42 0.50 0.63 0.79 0.99

The Ground-Layer Contribution

Tokovinin Thomas-Osip et al.Ground-Layer

Mauna Kea Ground Layer ~ 30m (Chun et al. 2009)LCO Ground Layer

~200-300m

32MooSci (TAMU) will further characterize LCO Ground Layer

Some Things to Consider This WeekHow do we build scientific bridges to LSST?

With the astro2010 competition over, now is the time to think about synergy

How does GMT work best with JWST?

Where do we compete, where do we complement and where should fear to tread?

When is the science case “good enough”

The role of the science case is evolving – how do we balance specific science with discovery space considerations?

How do we avoid locking in too soon?

Science is changing much faster than the time scale for technical development

New GMTO Website – Hosted at UT Austin – coming

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