GMT Instruments and AO. GMT Science Meeting - March
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1 GMT Instruments and AO GMT Science Meeting - March
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 GMT Science Meeting - March
3 Instrument Concepts Instrument Function λ range (microns) Resolution FOV GMACS NIRMOS QSpec SHARPS GMTNIRS MIISE HRCam GMTIFS Optical Multi-Object Spectrometer Near-IR Multi-Object Spectrometer Optical High Resolution Spectrometer Optical High Resolution (Doppler) Spectrometer Near-IR High-Resolution Spectrometer Mid-IR Imaging Spectrometer arcmin^ Up to ~ arcmin^ K 1 slit 3 + fibre mode K 7 x 1 fibers K-100K Single object Near-IR AO Imager NIR AO-fed IFU GMT Science Meeting - March
4 Adaptive Optics Modes Mode Description FOV Resolution Instruments GLAO LTAO NGSAO ExAO MCAO MOAO Ground Layer Adaptive Optics Laser Tomography Adaptive Optics Natural Guide Star Adaptive Optics Extreme Adaptive Optics Multi-Conjugate Adaptive Optics Multi-Object Adaptive Optics 7 arcmin 0.2 arcsec NIRMOS 30 arcsec 0.01 arcsec GMTIFS, HRCam 10 arcsec 0.01 arcsec MIISE, HRCAM 10 arcsec 0.01 arcsec HRCam 90 arcsec 0.01 arcsec TBD 10/90 arcsec 0.01 arcsec TBD GMT Science Meeting - March
5 Instrument Capabilities Resolving Power QSpec GMACS GMTNIRS GMTIFS NIRMOS MIISE Camera HRCam Wavelength (μm) GMT Science Meeting - March
6 Accommodating Wide-Field and Narrow-Field/AO Instruments GMT Science Meeting - March
7 Gregorian Instrument Mounting Large survey instruments mount below IP AO instruments - always hot above IP GMT Science Meeting - March
8 GMACS Visible Multi-Object Spectrometer GMT Science Meeting - March
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: 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 GMT Science Meeting - March
10 GMACS Optical Design x1 GMT Science Meeting - March
11 GMACS Optical Layout x4 GMT Science Meeting - March
12 GMACS Mechanical Layout 4 x 2 channel Field lens, slit mask, pick-off mirrors Mask changer Disperser changer GMT Science Meeting - March
13 NIRMOS Near-Infrared Multi-Object Spectrometer GMT Science Meeting - March
14 NIRMOS Overview Wavelength range: μm Imaging Mode: 7 x 7 arcmin field of view 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 GMT Science Meeting - March
15 NIRMOS Opto-Mechanical Layout GMT Science Meeting - March
16 GMACS/NIRMOS Interchangability GMACS active NIRMOS active GMT Science Meeting - March
17 Upper Instrument Platform Instruments GMT Science Meeting - March
18 Upper Instrument Platform 10 m x 16.5 m GMT Science Meeting - March
19 QSpec Visible High Resolution Spectrometer GMT Science Meeting - March
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) GMT Science Meeting - March
21 QSpec Optical design Red: 536 to 734 nm NIR: 723 to 1072 nm 1 m UV: 299 to 389 nm Blue: 383 to 545 nm GMT Science Meeting - March
22 QSpec on Instrument Platform GMT Science Meeting - March
23 Gravity-Invariant QSpec on C-Ring GMT Science Meeting - March
24 SHARPS Super HARPS GMT Science Meeting - March
25 SHARPS Overview Planet Doppler spectroscopy Fiber-fed: 7x (obj, sky, cal) x 1.0 arcsec fibers Resolving power ~ 150,000 Wavelength: > Å White pupil spectrograph design CCD mosaic detector Deep depletion CCDs for red orders Vacuum-enclosed spectrograph High-stability thermal environment Bulky enclosure GMT Science Meeting - March
26 SHARPS Optical Layout GMT Science Meeting - March
27 SHARPS at Coudé Feed GMT Science Meeting - March
28 GMTNIRS GMT Near-Infrared Spectrometer GMT Science Meeting - March
29 GMTNIRS Overview Short Wavelength: 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 GMT Science Meeting - March
30 GMTNIRS Optical Layout Short Wavelength Long Wavelength tertiary fpa cross-disperser tertiary FPA secondary primary paraboloid echelle primary cross disperser echelle paraboloid collimator slit fold paraboloid from GMT Cold pupil mm Scale: 1/ mm Scale: 1/8 GMT Science Meeting - March
31 GMTNIRS Mechanical Layout GMT Science Meeting - March
32 GMTNIRS on Instrument Platform GMT Science Meeting - March
33 Adaptive Optics Instruments GMT Science Meeting - March
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: arcsec at 1.0 μm arcsec at 2.0 μm arcsec at 4.0 μm 3x better than Gemini GMT Science Meeting - March
35 Scientific Impact of Images LTAO in the H band, 1 hr exposure, Antennae at z=1.4 GMT Science Meeting - March
36 Latest AO Reimaging Concept GMT Science Meeting - March
37 AO System on Instrument Platform LGS WFS GMT Science Meeting - March
38 MIISE Mid-Infrared Imaging Spectrometer GMT Science Meeting - March
39 MIISE Overview Wavelength range: 3-25 μm Field of view: arcsec Resolving power: R ~ 1500 Modes: Imaging Spectroscopy Nulling (8-25 μm) Coronography (3-5 μm) Short wavelength channel: 3-5 μm, arcsec/pixel Long wavelength channel: 8-25 μm, arcsec/pixel GMT Science Meeting - March
40 MIISE Optical Design dichroic 3-5 micron detector 8-25 micron detector input from AO feed nulling channel long wavelength imaging channel 2 micron phase sensor GMT Science Meeting - March
41 MIISE Location at Direct Focus GMT Science Meeting - March
42 GMTIFS GMT Integral-Field Spectrograph GMT Science Meeting - March
43 GMTIFS Overview Single-object, AO-corrected, integral-field spectroscopy Wavelength range: μm Resolving power: R = Range of spatial sampling and fields of view: Galaxy dynamics: arcsec sampling, 2-3 arcsec FOV Black hole masses: Diffraction-limited sampling, small FOV Spaxel size along slit (arcsec) Slitlet width (arcsec) Field of view (arcsec) GMT Science Meeting - March
44 GMTIFS Optical Layout Pupil Mirror Field Mirror Slicer Window Telescope Focus F-converter Collimator Image plane Pupil plane Grating Camera Fold Detector GMT Science Meeting - March
45 AO System on Instrument Platform LGS WFS GMT Science Meeting - March
46 HRCam High Resolution Camera GMT Science Meeting - March
47 HRCam Overview Wavelength range: μm Sampling: (f/46) and (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 arcsec/spaxel Resolving power: R ~ GMT Science Meeting - March
48 HRCam Optical Layout GMT Science Meeting - March
49 Still to be developed GMT Science Meeting - March
50 Optical Reimaging Camera GMT Science Meeting - March
51 Multiple Integral Field Spectroscopy ~ 10 IFUs MOAO-fed R ~ spaxels GMT Science Meeting - March
52 Summary Wide range of work-house capabilities Will it address key science in 10 yr time? Which will be the 1 st generation instruments? Are we catering for 2 nd & 3 rd generation instruments? GMT Science Meeting - March
53 GMT Science Meeting - March
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