Upload
keefer
View
33
Download
0
Tags:
Embed Size (px)
DESCRIPTION
GMTIFS – An AO-Corrected Integral-Field Spectrograph and Imager for GMT. Peter McGregor The Australian National University. Giant Magellan Telescope. GMT – Seven 8.4-m Segments. GMT First-Light Instrument Studies. Wide-field instruments. LTAO instruments. Timeline. - PowerPoint PPT Presentation
Citation preview
GMTIFS – An AO-Corrected Integral-Field
Spectrograph and Imager for GMT
Peter McGregorThe Australian National University
1IFUs in the Era of JWST - October 2010
GIANT MAGELLAN TELESCOPE
IFUs in the Era of JWST - October 2010 2
IFUs in the Era of JWST - October 2010 3
GMT – Seven 8.4-m Segments
IFUs in the Era of JWST - October 2010 4
Instrument Function l range(microns)
ResolvingPower
FOV
GMACS Optical Multi-ObjectSpectrometer
0.35-1.0 250-4000 64-200arcmin2
NIRMOS Near-IR Multi-ObjectSpectrometer
1.0-2.5 Up to ~4000 49arcmin2
G-CLEF Optical High Resolution(Doppler) Spectrometer
0.4-0.7 150K 7 x 1” fibers
GMTNIRS Near-IR High-ResolutionSpectrometer
1.2- 5.0 25K-100K Single object
GMTIFS NIR AO-fed IFU+Imager 0.9-2.5 5000-10000 <5”
TIGER Mid-IR ImagingSpectrometer
3.0-25.0 1500 30”
GMT First-Light Instrument Studies
Wide-field instruments LTAO instruments
IFUs in the Era of JWST - October 2010 5
Timeline
• Sept 2011: Six Conceptual Design Reviews• Oct 2011: Down select to 2-3 first-light instruments
• 2020: GMT first light
What will we want to be doing in 10 yr time?
LASER TOMOGRAPHY ADAPTIVE OPTICS
IFUs in the Era of JWST - October 2010 6
IFUs in the Era of JWST - October 2010 7
Laser Tomography Adaptive OpticsLTAO in the H band, Antennae at z=1.4
12 mas FWHM at 1.2 μm16 mas FWHM at 1.6 μm22 mas FWHM at 2.2 μm
IFUs in the Era of JWST - October 2010 8
Adaptive Secondary Mirror (ASM)
Hexapod
Interface
Telescope structure
Controller
Wind shield
DM assembly• Cold plate• Reference
Body• Face sheet
IFUs in the Era of JWST - October 2010 9
LTAO System LayoutLGS Projector
Laser beam relay
Laser house
Adaptive secondary mirror (ASM)
AO Focal Plane Assembly (FPA)
• Tertiary mirror• AO instruments• Optical TTF + Truth WFS• LGS wave-front sensors• Phasing camera
top view
GMTIFS SUMMARY
IFUs in the Era of JWST - October 2010 10
Motivations
• AO-corrected integral-field spectroscopy allows study of • Kinematics• Excitation
• GMT provides higher angular resolution for diffraction-limited science• Black-hole masses, protoplanetary disks• ~22 mas FWHM at 2.2 μm
• GMT provides larger collecting area for faint-object science• Galaxy dynamics at high redshift• 50 mas sampling, 4.5x2.24 arcsec FOV
IFUs in the Era of JWST - October 2010 11
Physical processes
GMTIFS – Overview
• Near-infrared; 1-2.5 μm + LTAO• Primary science instrument
• Single-object, LTAO-corrected, integral-field spectroscopy• Two spectral resolutions: R = 5000 (Δv = 60 km/s) & 10000 (Δv = 30 km/s) • Range of spatial sampling and fields of view:
• Secondary science instrument • Narrow-field, LTAO-corrected, imaging camera• 5 mas/pixel, 20.4× 20.4 arcsec FOV• Acquisition camera for IFS
• NIR AO-corrected tip-tilt WFS• 180 arcsec diameter guide field
• Flat-field and wavelength calibrationIFUs in the Era of JWST - October 2010 12
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
Guide Field Geometry
IFUs in the Era of JWST - October 2010 13
SCIENCE DRIVER The Formation of Disk Galaxies at High Redshift
IFUs in the Era of JWST - October 2010 14
High-z Disk Galaxies
IFUs in the Era of JWST - October 2010 15Elmegreen et al. (2009)
ClumpCluster
EarlyBulge
FlocculentSpiral
MatureSpiral
Natascha Förster-Schreiber
Marie Lemonie-Busserolle
Shelley Wright
Andy Green
IFUs in the Era of JWST - October 2010 16
Gravitationally Lensed Galaxies
MACS J2135-0102, z = 3.075
Stark et al. 2008, Nature, 455, 775
Tucker Jones
SCIENCE DRIVER “AGN” Feedback at High Redshift
IFUs in the Era of JWST - October 2010 17
[O III] in Radio Galaxies & ULIRGS
IFUs in the Era of JWST - October 2010 18
Nesvadba 2009; z ~ 2 radio galaxies
Alexander et al. 2010; z ~ 2 ULIRG SMM J1237+6203
SCIENCE DRIVER Massive Nuclear Black Holes
IFUs in the Era of JWST - October 2010 19
Nuclear Black Holes
IFUs in the Era of JWST - October 2010 20Graham (2008)
21
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 ~ 16 mas• 10 pc @ z = 0.04• 35 pc @ z = 0.15
• > 5×109 M☼ can be resolved at any distance
• 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
IFUs in the Era of JWST - October 2010
22
Massive Nuclear Black Holes
• Stellar kinematics of quasar host galaxies?• QSO PG1426+0.15 with NIFS (Watson et al. 2008, ApJ,
682, L21)
IFUs in the Era of JWST - October 2010
Nuclear Star Clusters
IFUs in the Era of JWST - October 2010 23Scarlata et al. (2004)
5"
SCIENCE DRIVER Active Galactic Nuclei
IFUs in the Era of JWST - October 2010 24
NGC 4151 - Seyfert 1 Galaxy
IFUs in the Era of JWST - October 2010 25
[Fe II] 1.644 μm H2 1-0 S(1) 2.122 μm
H I Brγ 2.166 μm [Ca VIII] 2.321 μmThaisa Storchi-Bergmann
João Steiner
SCIENCE DRIVER Protoplanetary Disks and Outflows from Young Stars
IFUs in the Era of JWST - October 2010 26
Protostellar Disks and Outflows
IFUs in the Era of JWST - October 2010 27
Tracy Beck
IFUs in the Era of JWST - October 2010 28
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
• 4 AU resn. with GMT at diffraction limit
100 AU
1 yr at 200 km/s
20 AU
INSTRUMENT DESIGN
IFUs in the Era of JWST - October 2010 29
LGS WFS
NGS WFS
GMTIFS Light Paths
IFUs in the Era of JWST - October 2010 30
AO WFSs GMTIFS
NIR NGS WFS
IFS
F-converters
Imager
Calibration Dichroic
OptLGSNIR
ADC
Optics – Trimetric View
IFUs in the Era of JWST - October 2010 31
Calibration system
Tertiary mirror
Imager
Spectrograph
First Satisfied Observer!
32
LTAO wave-front sensors
GMTIFS calibration system GMTIFS cryostat
IFUs in the Era of JWST - October 2010
GMTIFS on Instrument Platform
33IFUs in the Era of JWST - October 2010
SYNERGIES
IFUs in the Era of JWST - October 2010 34
IFUs in the Era of JWST - October 2010 35
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)
• 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
1 1.2 1.4 1.6 1.8 2 2.2 2.4-20.00
-19.00
-18.00
-17.00
-16.00
-15.00
-14.00
-13.00
Wavelength [microns]
Continuum Sensitivity: 10:1 in 10,000s
IFUs in the Era of JWST - October 2010 36
6 mas; R=10000
6 mas; R=5000
12 mas; R=10000
12 mas; R=5000
25 mas; R=1000025 mas; R=500050 mas; R=1000050 mas; R=5000
JWST; R=2700
AB mag/arcsec2
NIFS; R=5000
1 1.2 1.4 1.6 1.8 2 2.2 2.4
3.33E-17
3.33E-16
3.33E-15
Wavelength [microns]
Line Sensitivity: 200 km/s,10:1 in 10,000s
IFUs in the Era of JWST - October 2010 37
JWST; R=2700
6 mas; R=100006 mas; R=5000
12 mas; R=1000012 mas; R=500025 mas; R=1000025 mas; R=500050 mas; R=1000050 mas; R=5000
erg/s/cm2/arcsec2
NIFS; R=5000
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
IFUs in the Era of JWST - October 2010 38