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?

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What is the Gemini Near-infrared Integral Field
Spectrograph?
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Near Diffraction-Limited Imaging Spectroscopy
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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

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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
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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

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NIFS Optical Design
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Concentric IFU Design
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Concentric IFU Rays
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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

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Optical Throughput
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Optical Error Budget
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Rockwell 2048?2048 HAWAII-2
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Temperature Control Test System
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CdZnTe Technology
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4.75 ?m Cut-off Test Results
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Optimal Spectral Resolving Power
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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
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Guide Star Availability

• Observations of unique objects will be
  difficult
• Best to choose objects near to bright stars

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LGS OIWFS Star Availability

• Need OIWFS star with Rlt 16-19 mag within 30?
  radius.

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Expected Strehl Width
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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

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NGC 7469 CFHT AOB, K band
10 ?
0.13? FWHM
0.7? FWHM
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Seyfert Galaxy Sensitivities
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Seyfert Galaxy Sensitivities

• 3? per pixel in 3600 s at
• R 5500 and 500 km s-1
• line width

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Guide Star Availability
45 of 99 Seyfert galaxies tested have suitable
OIWFS stars.
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Redshifted Optical Emission-Lines
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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?
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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
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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
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Ultraluminous IR Galaxies Mrk 273
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Nearby Radio Galaxies Cygnus A
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QSO Host Galaxies?
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QSO J 18, z 1, J2 spectrum
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How does NIFS fit within the On-Going
Instrumentation Plan?
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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)

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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

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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

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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

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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

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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

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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
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• 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

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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)

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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)

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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)

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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)

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ALTAIR Adaptive Optics System
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Angular Anisoplanatism
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MCAO Tomography Cone Effect
(Focal Anisoplanatism)
90 km
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MCAO Tomography Cone Effect
(Focal Anisoplanatism)
90 km
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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

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MCAO Science
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MCAO Science
Star formation histories of physically
distinct components apparently vary - dynamical
data are essential.
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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)

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Future Instrumentation Plan
Gemini-North
2007
2008
2009
Gemini-South
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Related Instrumentation PhD Topics

• DBS Integral Field Unit
• Orthogonal Transfer CCD
• 40 inch Telescope Automation

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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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