The Giant Magellan Telescope
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1 The Giant Magellan Telescope Wendy Freedman Carnegie Observatories Chair, GMT Board Texas A&M Mitchell Symposium April 12, 2006
2 The Giant Magellan Telescope (GMT)
3 GMT Design Alt-az telescope structure Seven 8.4-m primary mirrors 24.5-m diffraction equivalent 21.5-m equivalent aperture
4 GMT Institutions Carnegie Observatories Harvard University Smithsonian Astrophysical Observatory Texas A&M University University of Texas, Austin University of Arizona University of Michigan Massachusetts Institute of Technology + OTHERS TBD
5 The GMT Why this group of institutions? More than 300 years of telescope building experience within the consortium Last telescope came in under budget
6 GMT Project Scientists Working Group Steve Shectman Carnegie Observatories Roger Angel U. Arizona Dan Fabricant Harvard/Smithsonian CfA Phillip MacQueen Paul Schechter MIT Matt Johns Carnegie Observatories Charles Jenkins Australia U. Texas at Austin Rebecca Bernstein U. Michigan
7 Science Working Group Warrick Couch Australia Xiaohui Fan Arizona Karl Gebhardt Texas Gary Hill Texas John Huchra Scott Kenyon Smithsonian Pat McCarthy (chair) Carnegie Michael Meyer Arizona Alycia Weinberger Carnegie/DTM Harvard
8 Telescope Structure & Optics Windshake: 4.5Hz lowest structural modes Height = 43 meters Rotating: 961 tons 7 x 8.4m Primary mirror segments + 1 spare off-axis segment.
9 The mirrors
10 Mold assembly for GMT Mirror 1 Tops of boxes follow shape of aspheric surface; no two are identical. Machine and install 1681 ceramic fiber boxes in silicon carbide tub.
11 Loading the Glass Close furnace: melt and spin. Inspect, weigh, and load 18 t of E6 borosilicate glass.
12 Casting First Off-Axis Segment: July 2006 Heat to 1160 C, spin at 4.9 rpm, hold 4 hours to allow glass to fill mold. Cool rapidly to 900 C then slowly for 3 months, 2.4 K/day through annealing ( C). First GMT off-axis segment
13 Lift and washout Removal of floor tiles Segment with lifting fixture Tilted into vertical plane Rear surface with floor tiles attached
14 Stressed Lap Polishing Machines at SOML Test tower LOG Stressed lap
15 New test tower at Mirror Lab * Needed for 8.4 m off-axis segments * Long 36 m radius of curvature (LBT = 20 m) * Requires diffraction limited 4 m folding spherical mirror at top
16 Segmented Adaptive Gregorian Secondary Mirror Technology developed for MMT & LBT 7 Segments aligned with Primary mirror segments attached to a single reference body. ~672 actuators per segment ~4700 actuators total 64 cm MMT AO secondary mirror
17 GMT Secondary Mirrors
18 Baseline Adaptive Optics Modes 1) Ground Layer AO covering 8 diameter field at the direct Gregorian focus ( μm) 2) Laser Tomography AO providing high-strehl, diffraction-limited correction across a 1 to 4 diameter field at folded Gregorian focii on the instrument platform ( μm) 3) Extreme Contrast AO optimized for the detection of planetary disks and young, hot planets with dedicated instruments on the instrument platform
19 Scientific Impact of Images: LTAO in the H band
20 First Generation Instrument Concepts Instrument λ(μm) Resolution FOV Modes Visible WF MOS NIR MOS Visible Echelle MOS, Imager MOS/IFU Imager 20K - 100K 20 Single Object Fiber feed NIR Echelle K-150K 30 Single Object MIR AO Imager NIR AO Imager x 2 Coronagraph Nulling int ``Wide-field & high definition modes
21 GMT Instrument Platform (IP) Rotator GLAO Guider Folded port instruments Echelle AO imager Gregorian instruments Optical capacity MOS Near-IR 6.4 m Dia. MOS 7.6 m high Mid-IR 25 Spectrograh ton
22 Carousel Enclosure 60 m C. Hull 54 m
23 Enclosure Structure M3 Engineering
24 Site Testing Northern Chile sites GMT conducting tests at 4 LCO sites Coordinate/share data with other projects Test equipment Differential Image Motion Monitors (DIMM) Meteorological stations Multi-aperture Scintillation Sensor (MASS) All-sky camera Precipitable Water Vapor Magellan (Manqui) Campanas Pk. Alcaino Pk. Ridge (Manquis)
25 Light Pollution Source: Calculation of light pollution based on satellite imagery obtained in Lowest contours indicate 1-10% increase over natural sky brightness
26 Examples of MASS/DIMM Data Phillips
27 Science with the Giant Magellan Telescope
28 Key Science Areas The First Stars and Galaxies Nature of Planets beyond our Solar System New Discoveries
29 Complementarity with JWST β Pic at 11μm JWST GMT JWST GMT 10 AU GMT has 4 times the spatial resolution. and up to 100 times the spectral resolution McCarthy
30 Origin and Evolution of Galaxies and Structure in the Universe CMB (WMAP image): seeds of galaxy and LSS formation 1. First light and reionization 2. Assembly of galaxies and clusters 3. Energetics of the IGM 4. Origin of the Hubble Sequence Sloan z > 6 quasar
31 Galaxy Assembly & First Light Star formation at z = 10 with GMT Barton et al With its wide field of view and enormous collecting area GMT will: Numerical simulation Probe star formation in the first billion years of cosmic time He II 1640 emission-line Image in H-band Gauge the formation of galaxies via the buildup of mass & heavy elements Explore the connection between galaxies and the intergalactic medium
32 Z = 6 with GMT Simulated 15 hr integration AΩ = 10 x DEIMOS
33 Galaxies and the IGM Simulated GMT spectrum of R = 24 galaxy at z = 2.4
34 Origins of Stars and Planets Large segments enable detection of extra-solar planets in reflected light 1. What determines stellar, browndwarf and planet mass functions? Radial velocity detection of planets 2. Environmental influence on planet formation process 3. Evolution from proto-planetary disks to planetary systems Circumstellar debris disk
35 Physical Properties of Extra-Solar Planets 1. Physics of planetary atmospheres Nulling interferometry at 10 μ m with Magellan 2. Survival of hot Jupiters 3. What are the distributions of planetary temperature, albedo, mass, size? GMT direct imaging GMT nulling interferometry Model spectra of giant planets
36 Planets and Their Formation With its superb angular resolution & sensitivity GMT will: Image known exoplanets in reflected light Discover young massive planets in nearby star forming regions Probe the structure of proto-planetary gas and debris disks
37 Can GMT carryout the NAS Decadal Survey Science case? Yes! Some parts take ~30-50% longer, others may be faster than the nominal GSMT What unique capabilities are offered by GMT? - Adaptive optics at the secondary - A unique PSF that is well suited to ExAO - Rapid instrument changes/too access - Wide-field GLAO - Wide-field spectroscopy without fibers
38 Schedule Milestones Contract for 1 st primary mirror segment 2004 Cast 1 st segment 2005 Complete conceptual design (review) 2006 Complete Preliminary Design (reviews) 2008/9 Complete 1 st segment 2008 Construction Phase Starts (assuming funding) 2009 First Light with 4 segments 2013 First science operation 2015 All 7 segments installed 2016
39 Toward Realizing the GMT Where are we now? First primary mirror cast successfully in July Conceptual Design completed Conceptual Design Review of Project February STRONG RECOMMENDATION TO PROCEED TO DDP! Beginning Polishing/Testing phase of Mirror I. Fundraising for Detailed Design in progress
40 Stay tuned!
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