instrumentation concepts for the 30-meter gsmt
DESCRIPTION
Instrumentation Concepts for the 30-meter GSMT. S.C. Barden, M. Liang, K.H. Hinkle, C.F.W. Harmer, R.R. Joyce (NOAO/NIO) September 17, 2001. GSMT Point Design Instrument Study. Develop telescope, AO and instruments as an integrated system Design concepts driven by science objectives - PowerPoint PPT PresentationTRANSCRIPT
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S.C. Barden, M. Liang, K.H. Hinkle, C.F.W. Harmer, R.R. Joyce (NOAO/NIO) September 17, 2001
Instrumentation Concepts for the 30-meter GSMT
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GSMT Point Design Instrument Study• Develop telescope, AO and instruments as an
integrated system• Design concepts driven by science objectives
– Multi-Object, Multi-Fiber, Optical Spectrograph MOMFOS (science: tomography of the universe)
– Near IR Deployable Integral Field Spectrograph NIRDIF (science: tomography of pre-galaxy fragments)
– Mid-IR, High Dispersion, AO Spectrograph MIHDAS (science: origins of planetary systems)
– MCAO-fed near-IR imager (science: stellar populations)
• Build on extant concepts where possible• Define major design challenges• Identify needed technologies
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Multi-Object Multi-Fiber Optical Spectrograph (MOMFOS)
• 20 arc-minute field at f/1 Prime Focus• 60-meter fiber cable• 700 0.7” fibers
• 3 spectrographs, ~230 fibers each• VPH gratings• Articulated collimator for different resolution regimes
Resolution Example ranges with single grating• R= 1,000 350nm – 650nm• R= 5,000 470nm – 530nm• R= 18,000 491nm – 508nm
• Detects 13% - 23% of photons hitting the 30m
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Prime Focus MOMFOS
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MOMFOS with Prime
Focus Corrector
Conceptual design fits in a 3m dia by 5m long cylinder
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MOMFOS Spectrograph Micro-Lens Relay
500 m diameterfiber fed by two micro-lenses with spherical surfaces.
100% of light couples into fiber.
Field stop limitslight to 0.72” aperture. Comparable lens required at fiber output.
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MOMFOS Spectrograph Fiber Positioner
Positioner based on Echidna positioner built by AAO for FMOS on Suburu
Echidna prototype image from www.aao.gov.au/local/www/echidna/
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MOMFOS Spectrograph
R=18000mode
R=5000mode
R=1000mode
500mm pupil; all spherical optics
4K by 4K CCD15 m pixels2 pixel binning
3 Spectrographs
230 fibers each
10 VPH gratingsto cover fulloptical rangeand 3 resolutionmodes.
f/4.5 Collimator
f/0.86 Camera
Articulatedcollimator
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MOMFOS Spectrograph Predicted Efficiency
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Spot Diagrams for MOMFOS Spectrograph
R = 50001126 l/mm794-904 nm28.6°
On-Axis
Half-Field
Full-Field
Fiber Diameter
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Tomography of Individual Galaxies out to z ~3
GSMT 3 hour, 3 limit at R=5,000
0.1”x0.1” IFU pixel0.1”x0.1” IFU pixel(sub-kpc scale structures)
J H K 26.5 25.5 24.0
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Near Infra-Red Deployable Integral Field Spectrograph (NIRDIF)
• MCAO fed• 1.5 to 2.0 arc-minute FOV
• 1 – 2.5 m wavelength coverage
• Deployable IFU units• 1.5 arc-second FOV per IFU probe• 31 slices per IFU probe (0.048” per slice)• ~26 deployable units
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Near Infra-Red Deployable Integral Field Spectrograph (NIRDIF)
Relay optics contained in deployable arm.
1.5 by 1.5 arc-second field of view.
f/38 to f/128 converter from MCAO field to imageslicer.
Telecentric input and output.
Cold stop located within relay.
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Near Infra-Red Deployable Integral Field Spectrograph (NIRDIF)
f/128 image slicer with 31 slices converted to f/11.5 for the spectrograph.
Spectrographs• 2 IFU’s per spectrograph• ~13 spectrographs• R = 1000 to 10,000• Z, J, H, and K spectral coverage• 2 K detector format assumed
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Near Infra-Red Deployable Integral Field Spectrograph (NIRDIF)
Image Relay
Image Slicer
Spectrograph
Two Image Slicers per Spectrograph
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Near Infra-Red Deployable Integral Field Spectrograph (NIRDIF)
Spot diagrams for NIRDIF spectrograph.
Slice 1
Slice 16
Slice 31
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Origins of Planetary Systems• Goals:
– Understand where and when planets form– Infer planetary architectures via observation of ‘gaps’
• Measurements:Spectra of accreting PMS stars (R~105; m)
• Key requirements:On axis, high Strehl AO; low emissivity
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Mid-Infrared High Dispersion AO Spectrograph (MIHDAS)
• Adaptive Secondary AO feed• On-Axis, Narrow Field/Point Source• R=120,000
• 3 spectrographs• 2-5 m (small beamed, x-dispersed), 0.2 arc-second slit length• 10-14 m (x-dispersed), 1 arc-second slit• 16-20 m (x-dispersed), 1 arc-second slit
• 10-14 m spectrograph likely to utilize same collimator as 16-20 m instrument. Different Gratings and Camera.
• 2-5 m spectrograph may require additional AO mirrors.
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Mid-Infrared High Dispersion AO Spectrograph (MIHDAS)
16-20 mm spectrograph will be large. Diffraction limitat 20 microns is about ¼ arc-second, comparable tonative seeing limit.
Echelle grating is 1.5 meters in length! Overall Overall instrument is expected to take up a instrument is expected to take up a volume of volume of about 4 by 2 by 3 meters!about 4 by 2 by 3 meters!
All of which needs to be cryogenically cooled.
Instrument to be located at Cass location and movewith the telescope.
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Mid-Infrared High Dispersion AO Spectrograph (MIHDAS)
1K by 1K Si:As detector27 m pixels
150 mm by 1500 mmR10 (84°) Echelle7 mm/line (0.143 l/mm)
f/18.75 Collimator
f/2 Camera
4-mirror camera
Off-axis paraboliccollimator
360 mm diametercross-disperser45 l/mm, 26.5° blaze
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MCAO Near-IR Imager• f/38 input with 1:1 reimaging optics
• 1.5 to 2 arc-minute field of view
Monolithic imager - 5.5 mm/arc-second plate scale! 0.004 arc-second per pixel sampling 685 mm sized detector array for 2 arc-min field! 28K by 28K detector! 7 by 7 mosaic of 4K arrays
Alternative approach is to have deployable capability for imaging over a subset of the total field.
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Instrument Locations on Telescope
MCAO-fedNIRDIForMCAO Imager
Cass-fedMIHDAS
Fiber-fedMOMFOS
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Information on AURA NIO activities is available at:
www.aura-nio.noao.edu