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GMTIFS – An AO-Corrected Integral-Field Spectrograph and Imager for GMT

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.

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GMTIFS – An AO-Corrected Integral-Field Spectrograph and Imager for GMT

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  1. GMTIFS – An AO-Corrected Integral-FieldSpectrograph and Imager for GMT Peter McGregor The Australian National University

  2. AO-Corrected IFS Adaptive Optics Integral Field Unit Spectrograph 1 kHz Δx = 6-50 mas Δv = 60 km/s GMT LTAO System GMTIFS GMT 2010 Korea - 2010 October 4-6

  3. Motivations GMT 2010 Korea - 2010 October 4-6

  4. 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 GMT 2010 Korea - 2010 October 4-6

  5. Motivation - GMT • Deliver better angular resolution withLaser 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 GMT 2010 Korea - 2010 October 4-6

  6. 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 arcsecdiam. guide field • Flat-field and wavelength calibration GMT 2010 Korea - 2010 October 4-6

  7. GMTIFS on Instrument Platform GMT 2010 Korea - 2010 October 4-6

  8. Science Drivers GMT 2010 Korea - 2010 October 4-6

  9. 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 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 GMT 2010 Korea - 2010 October 4-6

  10. 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 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 GMT 2010 Korea - 2010 October 4-6

  11. 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 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 GMT 2010 Korea - 2010 October 4-6

  12. The Formation of Disk Galaxies at High Redshift Science Driver GMT 2010 Korea - 2010 October 4-6

  13. High-z Disk Galaxies • Disk formation process • Rotational velocity vs velocity dispersion (Vrot/σ ~ 1-5 at z ~ 2) • Mass accumulation history • Hαdynamics • Star formation history • Hα luminosity • Chemical abundance history • Rest-frame optical emission-line ratios GMT 2010 Korea - 2010 October 4-6

  14. HUDF Chain Galaxies & Clump Clusters Chain Galaxies Clump Clusters Bulge Bulgeless ACS V NICMOS H ACS V NICMOS H Elmegreen et al. (2008) GMT 2010 Korea - 2010 October 4-6

  15. High-z Disk Galaxies Early Bulge Clump Cluster Mature Spiral Flocculent Spiral Elmegreen et al. (2009) GMT 2010 Korea - 2010 October 4-6

  16. GDDS-22 2172 with NIFS z = 1.563, 10 hr on Gemini North Hα 0.6563 [N II] 0.6583 1.0 arcsec GMT 2010 Korea - 2010 October 4-6

  17. Disk Galaxy at z=2.35; 6 x 900 s GMTIFSsim simulation HUDF - i GMT 2010 Korea - 2010 October 4-6

  18. Disk Galaxy at z=2.35; 6 x 900 s Vrot σ Line Central Intensity Continuum GMT 2010 Korea - 2010 October 4-6

  19. NIRSPEC (K) SINFONI/OSIRIS + AO GMTIFS - detectable GMTIFS – not detectable Line Luminosities Hα 6563 [O III] 5007 F(line) = 3x10-17 erg/s/cm2 [O II] 3727 Tresse et al. (2001) Erb et al. (2006) GMT 2010 Korea - 2010 October 4-6

  20. Massive Nuclear Black Holes Science Driver GMT 2010 Korea - 2010 October 4-6

  21. Nuclear Black Holes Graham (2008) GMT 2010 Korea - 2010 October 4-6

  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 104-106M☼ 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 GMT 2010 Korea - 2010 October 4-6

  23. High-Mass Black Holes • How massive do MBHs get (> 109 M☼)? • MBHvs L and MBHvsσ give disparate results • What is the space density of MBHs? > 5×109 M☼ from Karl Gebhardt GMT 2010 Korea - 2010 October 4-6

  24. 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 Watson et al. 2008, ApJ, 682, L21 Challenges of GMT Meeting - 2010 June 15-16

  25. Circumnuclear Gas Disks Cygnus A Pα 1.876 μm: 2×109 M☼ GMT 2010 Korea - 2010 October 4-6

  26. Nuclear Star Clusters Follow the black hole scaling relations Ferrarese et al. (2006) GMT 2010 Korea - 2010 October 4-6

  27. Low-Mass BlackHoles/Star Clusters 5" Scarlata et al. (2004) GMT 2010 Korea - 2010 October 4-6

  28. Protoplanetary Disks and Outflows from Young Stars Science Driver GMT 2010 Korea - 2010 October 4-6

  29. Protostellar Disks and Outflows GMT 2010 Korea - 2010 October 4-6

  30. 20 AU 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 GMT 2010 Korea - 2010 October 4-6

  31. 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! 2005 2006 2008 2010 2007 2004 2003 2009 GMT 2010 Korea - 2010 October 4-6

  32. DG Tau – Entrainment? -50 -100 -150 Bicknell (1984) GMT 2010 Korea - 2010 October 4-6

  33. Instrument Design GMT 2010 Korea - 2010 October 4-6

  34. GMTIFS Light Paths AO WFSs GMTIFS IFS NGS WFS F-converters Imager LGS WFS ADC Opt NIR NGS WFS LGS NIR Dichroic Calibration GMT 2010 Korea - 2010 October 4-6

  35. Maximal Cryostat Design GMT 2010 Korea - 2010 October 4-6

  36. NIR WFS Feed Compensator Tertiary Tip-tilt wave-front sensor Dichroic Window Field lens Beam-steering mirror GMT 2010 Korea - 2010 October 4-6

  37. Fore-Optics Layout Science fold mirror Rotating cold-stop mask Relay GMT 2010 Korea - 2010 October 4-6

  38. Imager Layout Relay Imager detector and focus stage Atmospheric Dispersion Corrector Imager utility wheel Imager filter wheels Imager feed GMT 2010 Korea - 2010 October 4-6

  39. IFS Layout IFS filter wheel IFS mask wheel IFS anamorphic focal ratio converters GMT 2010 Korea - 2010 October 4-6

  40. IFS Layout IFS grating wheel and steering mirrors IFS detector and focus stage IFS image slicer IFS pupil mirrors IFS collimator IFS field mirrors GMT 2010 Korea - 2010 October 4-6

  41. Optics – Trimetric View Calibration feed mirror Calibration system GMT 2010 Korea - 2010 October 4-6

  42. Calibration Subsystem LTAO wave-front sensors GMTIFS cryostat GMTIFS calibration system GMT 2010 Korea - 2010 October 4-6

  43. Synergies GMT 2010 Korea - 2010 October 4-6

  44. JWST Comparison • Integral-Field Spectroscopy: • GMTIFS will have higher spectral resolution (R = 5000-10000 vs 2700) • AND higher spatial resolution (≤ 50 masvs 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 GMT 2010 Korea - 2010 October 4-6

  45. 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 GMT 2010 Korea - 2010 October 4-6

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