gmtifs – an ao-corrected integral-field spectrograph and imager for gmt
DESCRIPTION
GMTIFS – An AO-Corrected Integral-Field Spectrograph and Imager for GMT. Peter McGregor The Australian National University. AO-Corrected IFS. Adaptive Optics. Integral Field Unit. Spectrograph. 1 kHz. Δx = 6-50 mas. Δv = 60 km/s. GMT LTAO System. GMTIFS. Motivations. - PowerPoint PPT PresentationTRANSCRIPT
GMTIFS – An AO-Corrected Integral-Field
Spectrograph and Imager for GMT
Peter McGregorThe Australian National University
AO-Corrected IFS
GMT 2010 Korea - 2010 October 4-6
Integral Field Unit SpectrographAdaptive Optics
GMT LTAO System GMTIFS
Δv = 60 km/sΔx = 6-50 mas
1 kHz
2
MOTIVATIONS
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Motivation - IFS
• AO-corrected integral-field spectroscopy was pioneered on 8-10m telescopes• NIFS on Gemini, SINFONI on VLT, OSIRIS on Keck• These have enabled “AO spectroscopy”
• It is now an essential feature on ~30 m telescopes• Imaging studies brightnesses, colors, morphology• Spectroscopy studies kinematics, excitation, physical processes
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Motivation - GMT
• Deliver better angular resolution with Laser Tomography Adaptive Optics (LTAO)• Diffraction-limited FWHM on GMT is ~ 16 mas at 1.6 μm• Black-hole masses, protoplanetary disks• Diffraction-limited sampling, small FOV
• Collect more light from faint objects• Partial AO correction, but not diffraction limit• Galaxy dynamics: 0.05 arcsec sampling, 3 arcsec FOV
• GMTIFS will benefit in both these ways
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GMTIFS – Overview
• Near-infrared; 1-2.5 μm• Single-object, AO-corrected, integral-field spectroscopy
• Primary science instrument• Two spectral resolutions: R = 5000 (Δv = 60 km/s) & 10000 (Δv = 30 km/s) • Range of spatial sampling and fields of view:
• Narrow-field, AO-corrected, imaging camera• Secondary science instrument• 5 mas/pixel, 20.4× 20.4 arcsec FOV• Acquisition camera for IFS
• NIR tip-tilt wave front sensor• 150 arcsec diam. guide field
• Flat-field and wavelength calibrationGMT 2010 Korea - 2010 October 4-6 6
Spaxel size (mas) 6 12 25 50
Field of view (arcsec) 0.54×0.27 1.08×0.54 2.25×1.13 4.5×2.25
GMTIFS on Instrument Platform
7GMT 2010 Korea - 2010 October 4-6
SCIENCE DRIVERS
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GMT 2010 Korea - 2010 October 4-6 9
GMT Science Drivers• Planets and Their Formation
• Imaging of exosolar planets• Radial velocity searches for
exoplanets• Structure and dynamics of proto-
planetary debris disks• Star formation and the initial mass
function• Stellar Populations and Chemical
Evolution• Imaging of crowded populations• Chemistry of halo giants in Local
Group galaxies
• Assembly of Galaxies• The mass evolution of galaxies• Chemical evolution of galaxies• Tomography of the inter-galactic
medium• Black Holes
• Mass determinations• Dark Energy and the Accelerating
Universe• Baryonic oscillations at z > 4• Supernovae at z > 1
• First Light and Reionization• The reionization era• First Light
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GMT Science Drivers• Planets and Their Formation
Imaging of exosolar planets• Radial velocity searches for
exoplanets Structure and dynamics of proto-
planetary debris disks Star formation and the initial mass
function• Stellar Populations and Chemical
Evolution Imaging of crowded populations• Chemistry of halo giants in Local
Group galaxies
• Assembly of Galaxies The mass evolution of galaxies Chemical evolution of galaxies• Tomography of the inter-galactic
medium• Black Holes
Mass determinations• Dark Energy and the Accelerating
Universe• Baryonic oscillations at z > 4 Supernovae at z > 1
• First Light and Reionization• The reionization era• First Light
GMT 2010 Korea - 2010 October 4-6 11
GMT Science Drivers• Planets and Their Formation
Imaging of exosolar planets• Radial velocity searches for
exoplanets Structure and dynamics of proto-
planetary debris disks Star formation and the initial mass
function• Stellar Populations and Chemical
Evolution Imaging of crowded populations• Chemistry of halo giants in Local
Group galaxies
• Assembly of Galaxies The mass evolution of galaxies Chemical evolution of galaxies• Tomography of the inter-galactic
medium• Black Holes
Mass determinations• Dark Energy and the Accelerating
Universe• Baryonic oscillations at z > 4 Supernovae at z > 1
• First Light and Reionization• The reionization era• First Light
SCIENCE DRIVER The Formation of Disk Galaxies at High Redshift
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High-z Disk Galaxies
• Disk formation process• Rotational velocity vs velocity dispersion (Vrot/σ ~ 1-5 at z ~ 2)
• Mass accumulation history• Hα dynamics
• Star formation history• Hα luminosity
• Chemical abundance history• Rest-frame optical emission-line ratios
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HUDF Chain Galaxies & Clump Clusters
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ACS V ACS VNICMOS H NICMOS H
Clump ClustersChain Galaxies
Bulge
Bulgeless
Elmegreen et al. (2008)
High-z Disk Galaxies
GMT 2010 Korea - 2010 October 4-6 15Elmegreen et al. (2009)
ClumpCluster
EarlyBulge
FlocculentSpiral
MatureSpiral
GDDS-22 2172 with NIFS
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α 0.
6563
[N II
] 0.
65831.0 arcsec
z = 1.563, 10 hr on Gemini North
Disk Galaxy at z=2.35; 6 x 900 s
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GMTIFSsim simulation HUDF - i
Disk Galaxy at z=2.35; 6 x 900 s
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Vrot σ
LineCentral
Intensity Continuum
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Line Luminosities
Tresse et al. (2001) Erb et al. (2006)
NIRSPEC (K)SINFONI/OSIRIS + AOGMTIFS - detectableGMTIFS – not detectable
F(line) =3x10-17
erg/s/cm2
Hα 6563
[O II] 3727[O III] 5007
SCIENCE DRIVER Massive Nuclear Black Holes
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Nuclear Black Holes
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22
Nuclear Black Holes• High spatial resolution is required at high-mass end
• R = GMBH/σ2 ~ 10.8 pc (MBH/108 M☼)(σ/200 km/s)-2
~ 35.3 pc (MBH/109 M☼)(σ/350 km/s)-2
• H-band diffraction limit = 0.014"• 10 pc @ z = 0.04• 35 pc @ z = 0.15
• High spectral resolution is required at low-mass end• Probe 104-106 M☼ black holes in clusters• Velocity dispersions ~ 20-60 km/s => FWHM ~ 40-140 km/s• Requires R ~ 10,000 (Δv ~ 30 km/s) to detect presence of
black hole
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23
High-Mass Black Holes
• How massive do MBHs get (> 109 M☼)?• MBH vs L and MBH vs σ give disparate results• What is the space density of MBHs?
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> 5×109 M☼
from Karl Gebhardt
Stellar Velocity Dispersion
• Stellar absorption features• CO Δv=2 at ~ 2.3 μm• CO Δv=3 at ~ 1.7 μm• Ca II triplet at ~ 0.85 μm
Challenges of GMT Meeting - 2010 June 15-16 24
Watson et al. 2008, ApJ, 682, L21
Circumnuclear Gas Disks
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Cygnus A Pα 1.876 μm: 2×109 M☼
Nuclear Star Clusters
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Follow the black hole scaling relations
Low-Mass BlackHoles/Star Clusters
GMT 2010 Korea - 2010 October 4-6 27Scarlata et al. (2004)
5"
SCIENCE DRIVER Protoplanetary Disks and Outflows from Young Stars
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Protostellar Disks and Outflows
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DG Tau – Integrated [Fe II] (2005)
• NIFS H band
• Inclination ~ 60°• > 5:1 jet aspect
ratio
• Launch radius expected to be ~ 1 AU
• 20 AU resolution with NIFS
• 3 AU resn. with GMT at diffraction limit
100 AU
1 yr at 200 km/s
20 AU
Protoplanetary Disks & Outflows
• DG Tau jet with NIFS• [Fe II] 1.644 μm
• One stationary clump
• One moving clump• 0.2 arcsec in 13 months• 130 km/s
• We will see changes in ~ 1 month with GMT!
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2007200620052004
2008
2009
2010
2003
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DG Tau – Entrainment?-50 -100 -150
Bicknell (1984)
INSTRUMENT DESIGN
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LGS WFS
NGS WFS
GMTIFS Light Paths
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AO WFSs GMTIFS
NIR NGS WFS
IFS
F-converters
Imager
Calibration Dichroic
OptLGSNIR
ADC
Maximal Cryostat Design
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NIR WFS Feed
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Tertiary
DichroicWindow
Compensator
Field lens
Beam-steering mirror
Tip-tilt wave-frontsensor
Fore-Optics Layout
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Science fold mirror
Relay
Rotating cold-stop mask
Imager Layout
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Relay
Atmospheric DispersionCorrector
Imager feedImager filterwheels
Imager utilitywheel
Imager detectorand focus stage
IFS Layout
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IFS mask wheelIFS anamorphic focal ratio converters
IFS filterwheel
IFS Layout
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IFS detectorand focus stage
IFS image slicer
IFS pupil mirrors
IFS field mirrors IFS collimator
IFS grating wheel and steering mirrors
Optics – Trimetric View
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Calibration system
Calibration feed mirror
Calibration Subsystem
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LTAO wave-front sensors
GMTIFS calibration system GMTIFS cryostat
SYNERGIES
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JWST Comparison
• Integral-Field Spectroscopy:• GMTIFS will have higher spectral resolution (R = 5000-10000 vs
2700)• AND higher spatial resolution (≤ 50 mas vs 100 mas)• AND GMTIFS may have lower read noise (??? vs ~ 5 e)
• GMTIFS will address broader science
• Imaging:• JWST will out-perform GMTIFS for imaging targets with 6.5 m
diffraction-limited resolution (85 mas @ K)• GMTIFS’s advantage is in observations requiring higher spatial
resolution (22 mas @ K)• Crowded fields, morphology, size measurement
• GMTIFS will do different science
Summary
• GMTIFS will be a general-purpose AO instrument for GMT
• It will address many of the key science drivers for GMT
• It will be competitive with similar instruments on other ELTs• (within certain caveats)
• It will fully utilize the LTAO capabilities of GMT
• It may be able to address key science (galaxy evolution) without phasing the seven M1 segments
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