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GMT Science Meeting - March 2008 1
GMT Instruments and AO
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GMT Science Meeting - March 2008 2
Instrument Status
• Scientific priorities have been defined• Emphasis on:
• Wide-field survey science (cosmology)• High resolution spectroscopy (abundances, Doppler planets)• Adaptive optics (planets, star formation, galaxy dynamics)
• Limited imaging capability• Queue-mode operating model adopted• Eight instrument concepts have been proposed• At different levels of development• Conceptual design studies are required• Down select will occur for ~ 3 first-light instruments
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GMT Science Meeting - March 2008 3
Instrument ConceptsInstrument Function λ range
(microns)Resolution FOV
GMACS
NIRMOS
Optical Multi-ObjectSpectrometer
0.35-1.0 250-4000 64-200arcmin^2
Near-IR Multi-ObjectSpectrometer
1.0-2.5 Up to ~4000 49arcmin^2
QSpec
SHARPS Optical High Resolution(Doppler) Spectrometer
0.4-0.7 150K 7 x 1” fibers
GMTNIRS
MIISE
HRCam
GMTIFS
Optical High ResolutionSpectrometer
0.3-1.05 30K1” slit
3” + fibre mode
Near-IR High-ResolutionSpectrometer
1.2- 5.0 25K-100K Single object
Mid-IR ImagingSpectrometer
3.0-25.0 1500 30”
Near-IR AO Imager 0.9-5.0 5-5000 30”
NIR AO-fed IFU 0.9-2.5 3000-5000 3”
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GMT Science Meeting - March 2008 4
Adaptive Optics Modes
Mode Description FOV Resolution Instruments
GLAO
LTAO
Ground LayerAdaptive Optics
7 arcmin 0.2 arcsec NIRMOS
Laser TomographyAdaptive Optics
30 arcsec 0.01 arcsec GMTIFS,HRCam
NGSAO
ExAO Extreme AdaptiveOptics
10 arcsec 0.01 arcsec HRCam
MCAO
MOAO
Natural Guide StarAdaptive Optics
10 arcsec 0.01 arcsec MIISE,HRCAM
Multi-ConjugateAdaptive Optics
90 arcsec 0.01 arcsec TBD
Multi-Object Adaptive Optics
10/90 arcsec 0.01 arcsec TBD
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GMT Science Meeting - March 2008 5
GMTNIRS
Instrument Capabilities
Wavelength (μm)1.0 10.00.3
Res
olvi
ng P
ower
5000
5000
050
0
5.0
HRCam
MIISE
GMTIFS
GMTNIRS
GMACSNIRMOS
QSpec
“Camera”
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GMT Science Meeting - March 2008 6
Accommodating Wide-Field and Narrow-Field/AO Instruments
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GMT Science Meeting - March 2008 7
Gregorian Instrument Mounting
• Large survey instruments mount below IP
• AO instruments - always “hot” – above IP
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GMT Science Meeting - March 2008 8
GMACS – Visible Multi-Object Spectrometer
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GMT Science Meeting - March 2008 9
GMACS – Overview
• Multi-object, multi-slit spectrograph• 4x spectrographs, each with blue and red arms• Field of view: 8 x 18 arcmin (~ 200 x 5 arcsec slits)• Wavelength range: 0.36 – 1.02 μm• Resolving power with 0.7 arcsec slit:
• R ~ 1400 in blue (215 km/s)• R ~ 2700 in red (110 km/s) (for accurate sky subtraction)• Cross-over at 6500 Å
• Collimated beam diameter: 300 mm• No direct imaging capability
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GMT Science Meeting - March 2008 10
GMACS – Optical Design x1
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GMT Science Meeting - March 2008 11
GMACS – Optical Layout x4
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GMT Science Meeting - March 2008 12
GMACS – Mechanical Layout
Mask changer4 x 2 channelField lens, slit mask, pick-off
mirrors
Disperser changer
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GMT Science Meeting - March 2008 13
NIRMOS – Near-Infrared Multi-Object Spectrometer
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GMT Science Meeting - March 2008 14
NIRMOS – Overview
• Wavelength range: 0.85 – 2.5 μm• Imaging Mode:
• 7 x 7 arcmin field of view• 0.067 arcsec/pixel• 6kx6k detector
• Spectroscopy Mode:• Multi-slits: 140 x 3 arcsec long, full λ coverage• 5 x 7 arcmin field of view• R ~ 3000 with 0.5 arcsec slits
• Augmented by GLAO
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GMT Science Meeting - March 2008 15
NIRMOS – Opto-Mechanical Layout
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GMT Science Meeting - March 2008 16
GMACS/NIRMOS InterchangabilityGMACS active NIRMOS active
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GMT Science Meeting - March 2008 17
Upper Instrument PlatformInstruments
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GMT Science Meeting - March 2008 18
Upper Instrument Platform10 m x 16.5 m
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GMT Science Meeting - March 2008 19
QSpec – Visible High Resolution Spectrometer
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GMT Science Meeting - March 2008 20
QSpec – Overview
• Four beam instrument• 450 mm beam diameter• R4 echelle gratings (x2): 200 x 1600 mm• Rφ = 30,000 arcsecs• λλ = 300 nm to 1.07 µm (in four channels)• 2-pixel resolving power is R=125,000• Pupil anamorphism• White pupil design• VPH grating cross-dispersion• Four catadioptric cameras• 4k x 6.5k to 6k x 8k CCDs (with 15 µm pixels)
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GMT Science Meeting - March 2008 21
QSpec – Optical design
UV: 299 to 389 nm Blue: 383 to 545 nm
NIR: 723 to 1072 nmRed: 536 to 734 nm
1 m
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GMT Science Meeting - March 2008 22
QSpec on Instrument Platform
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GMT Science Meeting - March 2008 23
Gravity-Invariant QSpec on C-Ring
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GMT Science Meeting - March 2008 24
SHARPS – Super HARPS
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GMT Science Meeting - March 2008 25
SHARPS – Overview
• Planet Doppler spectroscopy• Fiber-fed: 7x (obj, sky, cal) x 1.0 arcsec fibers• Resolving power ~ 150,000• Wavelength: > 4400 – 6700 Å• White pupil spectrograph design• CCD mosaic detector• Deep depletion CCDs for red orders• Vacuum-enclosed spectrograph• High-stability thermal environment• Bulky enclosure
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GMT Science Meeting - March 2008 26
SHARPS – Optical Layout
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GMT Science Meeting - March 2008 27
SHARPS at Coudé Feed
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GMT Science Meeting - March 2008 28
GMTNIRS – GMT Near-Infrared Spectrometer
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GMT Science Meeting - March 2008 29
GMTNIRS – Overview
• Short Wavelength:• 1.2 – 2.4 μm (H & K covered in a single exposure)• Slit-limited resolving powers:
• R = 50,000, 0.3 arcsec slit ≡ 6 pixels• R3 immersion echelle grating• f/3 camera => 14 arcsec per order• 4096x4096 detector => 15 orders at K
• Long Wavelength (with AO):• 2 – 5 μm wavelength range• Diffraction-limited resolving powers:
• λ = 3.6 μm, R = 133,000, 0.06 arcsec slit ≡ 3 pixels• λ = 4.8 μm, R = 100,000, 0.08 arcsec slit ≡ 4 pixels
• f/7.8 camera => 0.85 arcsec per order at L• 2048x2048 detector
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GMT Science Meeting - March 2008 30
GMTNIRS – Optical Layout
200.00mmScale: 1/8Cold pupil
paraboloid
paraboloid from GMT
paraboloidprimary
tertiary
fpa
echelle
cross-disperser
200.00 mmScale: 1/8
slit
echelle
collimator
fold
primarysecondary
FPA
tertiary
crossdisperser
Short Wavelength Long Wavelength
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GMT Science Meeting - March 2008 31
GMTNIRS – Mechanical Layout
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GMT Science Meeting - March 2008 32
GMTNIRS on Instrument Platform
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GMT Science Meeting - March 2008 33
Adaptive Optics Instruments
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GMT Science Meeting - March 2008 34
Adaptive Optics Concept
• Single DM with common wave front sensing
• Asterism of 6 laser guide stars• Variable extent on sky
• Adaptive Secondary Mirror• Straight-through path to GLAO• Dichroic folds to LTAO,
thermal NGS, & ExAO• Diffraction limit:
• 0.010 arcsec at 1.0 μm• 0.020 arcsec at 2.0 μm• 0.040 arcsec at 4.0 μm• 3x better than Gemini
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GMT Science Meeting - March 2008 35
Scientific Impact of 0.016″ ImagesLTAO in the H band, 1 hr exposure, Antennae at z=1.4
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GMT Science Meeting - March 2008 36
Latest AO Reimaging Concept
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GMT Science Meeting - March 2008 37
AO System on Instrument Platform
LGSWFS
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GMT Science Meeting - March 2008 38
MIISE – Mid-Infrared Imaging Spectrometer
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GMT Science Meeting - March 2008 39
MIISE – Overview
• Wavelength range: 3 - 25 μm• Field of view: 30 – 40 arcsec• Resolving power: R ~ 1500• Modes:
• Imaging• Spectroscopy• Nulling (8-25 μm)• Coronography (3-5 μm)
• Short wavelength channel: 3-5 μm, 0.010 arcsec/pixel• Long wavelength channel: 8-25 μm, 0.030 arcsec/pixel
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GMT Science Meeting - March 2008 40
MIISE – Optical Design
input fromAO feed
3-5 micron detector
8-25 micron detector
2 micronphase sensorlong wavelength
imaging channel
nulling channel
dichroic
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GMT Science Meeting - March 2008 41
MIISE – Location at Direct Focus
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GMT Science Meeting - March 2008 42
GMTIFS – GMT Integral-Field Spectrograph
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GMT Science Meeting - March 2008 43
GMTIFS – Overview
• Single-object, AO-corrected, integral-field spectroscopy• Wavelength range: 1.0 – 2.5 μm• Resolving power: R = 4000 – 5000• Range of spatial sampling and fields of view:
• Galaxy dynamics: 0.05-0.10 arcsec sampling, 2-3 arcsec FOV• Black hole masses: Diffraction-limited sampling, small FOV
Spaxel size along slit (arcsec) 0.008 0.016 0.032 0.054
Slitlet width (arcsec) 0.020 0.040 0.080 0.135
Field of view (arcsec) 0.80 1.6 3.2 5.4
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GMT Science Meeting - March 2008 44
GMTIFS – Optical Layout
Window TelescopeFocus
Imageplane
F-converter
Pupilplane
SlicerPupil Mirror Field Mirror
Collimator
FoldGrating Camera Detector
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GMT Science Meeting - March 2008 45
AO System on Instrument Platform
LGSWFS
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GMT Science Meeting - March 2008 46
HRCam – High Resolution Camera
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GMT Science Meeting - March 2008 47
HRCam – Overview
• Wavelength range: 1 – 2.5 μm• Sampling: 0.003 (f/46) and 0.010 (f/15) arcsec/pixel• Field of view: 13 (f/46) and 40 (f/15) arcsec• Detector: 4096x4096 pixels• Imaging:
• JHK + narrow bands• Sensitivity: Must reach H & K ~ 25 mag
• IFU spectroscopy: • 50x50 spaxels with 0.020 arcsec/spaxel• Resolving power: R ~ 3000 - 5000
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GMT Science Meeting - March 2008 48
HRCam – Optical Layout
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GMT Science Meeting - March 2008 49
Still to be developed…
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GMT Science Meeting - March 2008 50
Optical Reimaging Camera
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GMT Science Meeting - March 2008 51
Multiple Integral Field Spectroscopy
• ~ 10 IFUs• MOAO-fed• R ~ 4000• 0.1” spaxels
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GMT Science Meeting - March 2008 52
Summary
• Wide range of work-house capabilities• Will it address key science in 10 yr time?• Which will be the 1st generation instruments?• Are we catering for 2nd & 3rd generation instruments?
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