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Title: NIFS: Australias First Gemini Instrument


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NIFS Australias First Gemini Instrument
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NIFS Australias First Gemini Instrument
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Overview
  • What is NIFS?
  • What science will NIFS do?
  • How does NIFS fit within the On-Going
    Instrumentation Plan?
  • How does NIFS fit within Geminis long-term plans?

5
What is the Gemini Near-infrared Integral Field
Spectrograph?
6
Near Diffraction-Limited Imaging Spectroscopy
7
NIFS Design Goals
  • Near-infrared, integral-field spectrograph
  • Use with ALTAIR AO system
  • 3.0??3.0? field-of-view
  • R 5300 in J, H, and K photometric bands
  • HAWAII-2 2048?2048 HgCdTe detector
  • Largely fixed-format design
  • Fast-track design and construction
  • Re-use NIRI design
  • Cryostat
  • OIWFS
  • Mechanism control system
  • Thermal control system
  • EPICS software

8
Baseline Specification
  • Wavelength range 0.94-2.5 ?m
  • Spatial pixel size 0.04??0.10?
  • Spectral resolving power 5300 (two pixels)
  • Focal plane occulting masks 0.1?, 0.2?, 0.5?
    circular
  • Order blocking filters Z, J, H, K
  • Gratings Z, J, H, Ks,Kl.
  • Detector Rockwell 2048?2048 HAWAII-2
    HgCdTe/PACE
  • Near-infrared OIWFS
  • Wavelength range 0.95-2.5 ?m
  • Steerable over 180 ? FOV (120? with ALTAIR)
  • Image scale 0.170?/pixel
  • Filters J, H, K
  • Instantaneous FOV lt 10?

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Reflective Staircase Integral Field Unit
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Reflective Staircase IFU
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Mechanical Layout
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NIFS Cryostat
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OIWFS Parts
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Duplicate of NIRI Cryostat
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3D IFU Design
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Content IFU Design
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IFU Mechanical Design
18
Simulated K 15 mag star,
1800 s, K grating
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Sky-subtracted K 15 mag star, 1800 s, K grating
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Compressed image of K 15 mag star, Strehl
0.2, seeing FWHM 0.4?
y
?
x
  • 3.0??3.0? FOV
  • 0.1? wide slitlets
  • 0.04??0.1? spatial pixels
  • 2048 spectral pixels

21
NIFS Optical Design
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Concentric IFU Design
23
Concentric IFU Rays
24
Fore-Optics
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Opto-Mechanical Design
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Optical Components
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Optical Components
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Grating Wheel
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OIWFS Guide Star Field
  • Guide stars to 12.7? from science object
  • Bright stars may scatter into probe

30
Optical Throughput
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Optical Error Budget
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Rockwell 2048?2048 HAWAII-2
33
Temperature Control Test System
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CdZnTe Technology
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4.75 ?m Cut-off Test Results
36
Optimal Spectral Resolving Power
37
NIFS Baseline Gratings
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Point Source Performance Summary
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Extended Continuum Source Summary
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Extended Line Source Summary
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Performance Calculator
http//www.mso.anu.edu.au/nifs
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What science will NIFS do?
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NIFS Science
Is
ALTAIR Science
45
Guide Star Availability
  • Observations of unique objects will be
    difficult
  • Best to choose objects near to bright stars

46
LGS OIWFS Star Availability
  • Need OIWFS star with Rlt 16-19 mag within 30?
    radius.

47
Expected Strehl Width
48
M13 with Gemini
NIFSALTAIR 0.1? slitlets 3.0??3.0? FOV
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Science Drivers
  • Massive black holes. R 3000-5000
  • AGN in nearby galaxies. R 3000
  • Low mass stars. R 1000
  • Compact star clusters. R 2000
  • YSO jet mechanisms. R 3000-6000
  • YSO/cloud interactions. R 6000
  • Proto/planetary nebulae. R 6000
  • Galactic center. R 3000-4000
  • Stellar populations in nearby galaxies. R
    1000-3000
  • Starburst galaxies. R 3000-5000
  • ULIR galaxies. R 3000-5000
  • High redshift galaxies? R 4000-6000
  • Lyman break galaxies? R 4000-6000
  • QSO host galaxies? R 1000-3000

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Nearby Galactic Nuclei
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Circumnuclear Disks
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Galaxy at 10 Mpc, 3600s, K grating
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Galaxies to 20 Mpc and ? lt -40
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Nearby Galaxies
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Seyfert Galaxies
  • H2 FWHM 260 km s-1
  • Fe II FWHM 487 km s-1

56
NGC 7469 CFHT AOB, K band
10 ?
0.13? FWHM
0.7? FWHM
57
Seyfert Galaxy Sensitivities
58
Seyfert Galaxy Sensitivities
  • 3? per pixel in 3600 s at
  • R 5500 and 500 km s-1
  • line width

59
Guide Star Availability
45 of 99 Seyfert galaxies tested have suitable
OIWFS stars.
60
Redshifted Optical Emission-Lines
61
Disk Galaxies at z 1
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Which Galaxies to Study?
  • At z 1
  • FH? 3.5 ? 10-23 W cm-2
  • M(B) -20.5 mag

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Disk galaxy, H? in J2 grating, z 1.0, 3600 s
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H36587_1252 z 0.321 barred spiral
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H36566_1245 z 0.518 Sb spiral
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H36571_1225 z 0.561 Sc spiral
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F37167_1042 z 0.821 merger?
68
F37058_1153 z 0.904 2-arm spiral
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F37221_1210 z 0.928 debris field
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F36287_1023 z 0.936 merger
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H36555_1249 z 0.950 proto-spiral?
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F36336_1005 z 1.015 merger?/irregular
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H36444_1142 z 1.020 disk-like
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Lyman Break Galaxies
75
Galactic Center
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YSO Jet Mechanisms
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YSO Jet-Cloud Interaction
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H2 1-0 S(1) 10-20 W cm-2 arcsec-2
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YSO Jet Mechanisms
NICMOS H
NICMOS K
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YSO Jet Driving Mechanism
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Nearby Starburst Galaxies He2-10
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Ultra-Luminous Infrared Galaxies
83
Ultraluminous IR Galaxies Mrk 273
84
Nearby Radio Galaxies Cygnus A
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QSO Host Galaxies?
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QSO J 18, z 1, J2 spectrum
87
How does NIFS fit within the On-Going
Instrumentation Plan?
88
Initial Instrument Complement
  • Mauna Kea
  • Near IR Imager (NIRI)
  • Multi-Object Spectrograph (GMOS)
  • ALTAIR NGS AOS
  • Shared Instruments
  • Michelle (UKIRT)
  • Visitor Instruments
  • CIRPASS (Cambridge)
  • OSCIR (Florida)
  • Cerro Pachon
  • Multi-Object Spectrograph (GMOS)
  • Mid IR Imager (T-ReCS)
  • High Resolution Optical Spectrograph (HROS)
  • Near IR Spectrograph (GNIRS)
  • Shared Instruments
  • Phoenix (CTIO)
  • Visitor Instruments
  • FLAMINGOS (Florida)

89
Near Infrared Imager(NIRI)
  • University of Hawaii
  • Detector 1024x1024 InSb array with 27 µm pixels
  • 1-5.5?µm wavelength coverage
  • High Throughput
  • Three Plate Scales
  • Pixel Size Field of View
  • 0.02 21
  • 0.05 51
  • 0.12 123
  • Filters 20-30 slots for filters, grisms, and
    polarizers
  • Grism mode
  • Coronagraphic mode

90
Multi-Object Spectrograph(GMOS)
  • HIA/UK ATC
  • Two Instruments Gemini North and Gemini South
  • Detector 3 EEV CCDs with 2048x4608 13.5 µm
    pixels
  • Image Scale 0.08 arcsec/pixel (5.5 arcmin FOV)
  • Wavelength Range 0.36-1.10 µm
  • Slit Sampling 2.5 times the image pixel scale
  • Imaging Mode Supports MOS mask production
  • Spectral Resolution 500 - 10,000 with various
    gratings
  • Integral Field Mode 0.2 arcsec sub-apertures

91
Mid-Infrared Imager(T-ReCS)
  • University of Florida
  • Highest Priority for this Instrument is
    Broad-Band 10 µm Diffraction Limited Imaging
  • Low-moderate spectroscopy mode supported
  • Array 256x256 SiAs IBC
  • Wavelength Range 5 to 25 µm
  • Plate Scale 0.09 arcsec/pixel
  • Instrument Background lt 1 effective emissivity
  • Filters Cold filter wheel with 20-30 slots

92
Facility Adaptive Optics System(ALTAIR)
  • Herzberg Institute of Astrophysics
  • Mauna Kea baseline system is NGS with LGS upgrade
    path
  • Optimized for 1.0-2.5 µm
  • Feeds any instrument at Cass
  • Preserves plate scale and image plane location of
    basic telescope
  • Optical throughput of AO unit 90
  • H-band Strehl of end-to-end system 40
  • Bright star, 45 from zenith, median seeing

93
Calibration Unit (GCAL)
  • UK ATC
  • Spectral and flat field calibrations for
    instruments in the 0.3-5.0 µm range will be
    performed through a common calibration unit
  • Output uniform in the central 3 arcmin field to
    1
  • Preserves telescope pupil
  • Central science fold mirror used to feed Cal Unit
    flux to any instrument
  • No feed into AO unit available

94
High Resolution Optical Spectrograph(HROS)
  • University College London
  • Detector 2 EEV CCDs with 2048x4608 13.5 µm
    pixels
  • Throughput is highest Priority, particularly in
    UV
  • Requirement gt10 at R50,000 and 500nm goal
    20
  • Resolution 50,000
  • Sampling 3 Pixels per Resolution Element
  • Wavelength Coverage 0.3 - 1.0 µm total with
    essentially all of this range covered in a single
    exposure
  • Stability lt0.05 resolution element in one hour
    integration

95
Near Infrared Spectrometer(GNIRS)
  • NOAO
  • Detector 1024x1024 with 27 µm pixels
  • Wavelength coverage 0.9-5.5 µm
  • High Throughput
  • Spectral Resolution R 2000, 5400 18000
  • Pixel Scales 0.05 0.15 arcsec/pixel
  • Slit Lengths 50 or 100 arcsec
  • Cross Dispersion (1-2.5 µm)
  • Polarizing Prism
  • Integral Field Mode (Durham)

96
Near -infrared Integral Field Spectrograph(NIFS)
  • RSAA, ANU
  • Detector 2048x2048 HAWAII-2 with 18 µm pixels
  • Wavelength Coverage 0.9-2.5 µm
  • Used with ALTAIR Adaptive Optics System
  • Integral Field Unit FoV 3.0"?3.0"
  • Slitlet Width 0.1"
  • Pixel Scale 0.04" (spatial) ? 0.05" (spectral)
  • Spectral Resolution R 5400
  • Occulting Masks
  • Wire-Grid Polarizer (K band)

97
Other Instrument Developments
  • MK CP facility polarization units (GPOL)
  • MK laser beacon upgrade to ALTAIR
  • CP facility laser beacon AO
  • CP near-infrared Coronagraph/Imager (NICI)
  • MK near-infrared integral field spectrograph
    (NIFS)
  • CP near-infrared multi-slit spectrograph
    (FLAMINGOS-II)

98
Instrument Availability Summary(Dates indicate
first community access)
Gemini-North
Gemini-South
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How does NIFS fit within Geminis long-term plans?
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Future Instrumentation Plan
  • Mauna Kea
  • ALTAIR LGS System
  • Near IR Imager (NIRI)
  • Near IR Integral-Field Spectrograph (NIFS)
  • Cerro Pachon
  • Multi-Conjugate Adaptive Optics (MCAO)
  • Diffraction-Limited Near IR Imager (GIRCAM)
  • Multiple Deployable IFU Near IR Spectrograph
    (GIRMOS)

101
ALTAIR Adaptive Optics System
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Angular Anisoplanatism
103
MCAO Tomography Cone Effect
(Focal Anisoplanatism)
90 km
104
MCAO Tomography Cone Effect
(Focal Anisoplanatism)
90 km
105
MCAO Simulations
  • Numerical simulations
  • 5 Natural guide stars
  • 5 Wavefront sensors
  • 2 mirrors
  • 8 turbulence layers
  • MK turbulence profile
  • Field of view 1.2
  • H band

106
MCAO Science
107
MCAO Science
Star formation histories of physically
distinct components apparently vary - dynamical
data are essential.
108
Next Generation Telescopes
  • NGST (8 m)
  • NIR/Vis. camera
  • NIR MOS R 1000
  • MIR camera/slit spectrograph R 1500
  • NIR IFS
  • High res. Vis. camera
  • MIR IFS
  • CELT (30 m)
  • OWL (100 m)
  • MAXAT (50 m)

109
Future Instrumentation Plan
Gemini-North
2007
2008
2009
Gemini-South
110
Related Instrumentation PhD Topics
  • DBS Integral Field Unit
  • Orthogonal Transfer CCD
  • 40 inch Telescope Automation

111
Energy Sensitive Detector Development
  • Superconducting Tunnel Junctions
  • http//astro.estec.esa.nl/astrogen/stj/mission_to
    p.html

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Summary
  • NIFS science ? MCAO science ? MAXAT science
  • Planning NIFS science programs now
  • http//www.mso.anu.edu.au/nifs
  • peter_at_mso.anu.edu.au
  • MCAO Science Workshop Victoria, B.C., Sep/Oct
    2000

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Pictures of the telescopes!
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Central Acquisition Guidance System Beam
Director
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Instrument Support Structure
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