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GSMT SWG - Nov 8 & 9 2007 1
Science With the GMTP. McCarthy
GMT Science Working Group
GMT Board
• Status and strengths of the GMT
• Potential for national participation
• Example science use cases
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Context of the GMT Science Goals
Balance between wide-field and diffraction-limited science
• 25′ diameter fov,
• Viable corrector designs for up to 22′
• 10mas diffraction-limit at 1µm
• Gregorian secondary conjugates ~ 150m above primary mirror - ideal for ground-layer adaptive optics
• Adaptive secondary mirror provides low-background high StrehlAO modes as well as GLAO and the first DM for ExAO
Natural Strengths of the GMT Design
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First segment on the large optics grinder at the Steward mirror lab
Status of Primary Mirror Segments
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GSMT SWG - Nov 8 & 9 2007 4
LCO Selected as GMT Site in October 2007
Magellan (Manqui) Campanas Pk.
Alcaino Pk.
Ridge (Manquis)
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Instrument Concepts
McGregor1.5”3000-50000.9-2.5NIR AO-fed IFU
JaffeSingle obj20K-200K1.2- 5.0Near-IR High-ResolutionSpectrometer
Close30”5-50000.9-5.0Near-IR AO Imager
Hinz30′′20K-120K1.0-5.0Near-IR High-ResolutionSpectrometer
MacQueen3′′ + fibremode
45K1” slit
0.3-1.05Optical High ResolutionSpectrometer
Fabricant7′ x 7′1200-50001.0-2.5Near-IR Multi-ObjectSpectrometer
Shectman9′ x 10′2500-50000.35-1.0Optical Multi-ObjectSpectrometer
P.I.FOVResolutionλ range(microns)
Instrument
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Instrument Selection Timescale
Call for new and continuing concept studies Winter 07/08
Design reviews Spring 2009
Selection of first generation instruments Summer 2009
Detailed design and construction contracts Fall 2009
Second generation instruments defined Mid 2012
First instruments delivered to Chile Fall 2014
There remains time and opportunity for the community to be engaged inthe instrument development and selection process
GMT is open to considering complementarity with TMT in firstgeneration instrument suites
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Gregorian Instrument Mounting
Large survey instruments mount below
AO instruments - always “hot” - above
Rapid instrument changes, queue observing
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How much time could be available through federal participation?
25-30% NSF share ~ 80 - 100 nights
GMT use cases focused on ~ 3 - 10 night programs - suitable for a PhD thesis
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GMT Science Use Cases
Imaging of terrestrial planets and debris disks at 5 - 10µm
mid-IR AO imager
Bulge-Black hole mass relationship at high redshifts
GMT AO-fed IFU
Lyα luminosity function at z ~ 6
GMACS
Stellar content of galaxies at z ~ 2-3
NIRMOS
Dynamics of Galaxies at 1 < z < 3
Use cases are built around instrument-specific exposure time calculatorsand spectral simulators
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GMT Survey InstrumentsIMACS f/2
GMACS
NIRMOS
18′
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GSMT SWG - Nov 8 & 9 2007 11
Use Case: Lyα Luminosity Function at z ~ 6
GOAL: Measure the faint end of the Lyα luminosity function at z ~ 6 as a probe of the end of reionization
Instrument Used: GMT Wide-Field Optical Spectrograph - GMACS
Number of Nights: 4 in queue mode
Supporting observations: Deep imaging survey
Approach: multi-slit spectroscopy of Lyα emission lines
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Use Case: Lyα Luminosity Function at z ~ 6
Ly α luminosity functionfrom Malhotra & Rhoads
Wide-field NB imagingStrong Lensing
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Use Case: Lyα Luminosity Function at z ~ 6
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Use Case: Lyα Luminosity Function at z ~ 6
6986350-1.8640.5
2502300-2.3041.0
1491357-2.5341.2
70635-2.8641.5
18163-3.4542.0
329-4.2042.5
N(5.7 < z < 5.8)N(5 < z < 6)φ(α = -2)Log L(Lyα)
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Use Case: Lyα Luminosity Function at z ~ 6
35 hour integrationswith GMOS onGemini S. Faintestobjects haveF = 5E-18.
Stanway et al. 2006.
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Use Case: Lyα Luminosity Function at z ~ 6
500 km/s FWHM
Wλ = 100Å
30hr integration with GMACSusing 0.5” slits in 0.5” seeing
30% throughput
Gemini sky spectrum
Nod & Shuffle sky rejection
R = 5000 rebinned to
R = 1200, Gaussian smoothing
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Use Case: Lyα Luminosity Function at z ~ 6
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Use Case: Stellar Content of DRGs at z > 2
GOAL: Probe the role of feed-back in the genesis of massive galaxies. Near-IRspectra provide a probe of star formation histories, ages and abundances
Instrument Used: GMT Near-IR MOS - NIRMOS
Number of Nights: 4 in queue mode
Supporting observations: Existing near-IR imaging surveys
Approach: Multi-slit spectroscopy of passive galaxies in the J-band and star forming galaxies in the K-band
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GSMT SWG - Nov 8 & 9 2007 19
Current State of the Art
Kreik et al.
GNIRS
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Use Case: Stellar Content of DRGs at z > 2
2 magnitudes!
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Use Case: Stellar Content of DRGs at z > 2
290Total
75871625.0
70751124.5
6065624.0
5060323.5
3540123.0
N(4 nights)N(1 < z < 2)N(2 < z < 4)J(AB)
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Use Case: Stellar Content of DRGs at z > 2
Simulated GMT spectraof old galaxies at z = 2
R = 3000 rebinned to R =1200
7.5e- read noise
Median J-band seeing
0.45” FWHM
Five-hour integrations
900 second unit exposure
GLAO Correction!
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Use Case: Stellar Content of DRGs at z > 2
Erb et al.
3E-17
2E-17
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