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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. Giant Magellan Telescope. GMT – Seven 8.4-m Segments. GMT First-Light Instrument Studies. Wide-field instruments. LTAO instruments. Timeline.

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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 IFUs in the Era of JWST - October 2010

  2. Giant Magellan Telescope IFUs in the Era of JWST - October 2010

  3. GMT – Seven 8.4-m Segments IFUs in the Era of JWST - October 2010

  4. 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? IFUs in the Era of JWST - October 2010

  6. Laser Tomography Adaptive OptiCs IFUs in the Era of JWST - October 2010

  7. Laser Tomography Adaptive Optics LTAO in the H band, Antennae at z=1.4 12 mas FWHM at 1.2 μm 16 mas FWHM at 1.6 μm 22 mas FWHM at 2.2 μm IFUs in the Era of JWST - October 2010

  8. Adaptive Secondary Mirror (ASM) Telescope structure Interface Hexapod Wind shield • DM assembly • Cold plate • Reference Body • Face sheet Controller IFUs in the Era of JWST - October 2010

  9. top view LTAO System Layout LGS Projector Adaptive secondary mirror (ASM) Laser beam relay • AO Focal Plane Assembly (FPA) • Tertiary mirror • AO instruments • Optical TTF + Truth WFS • LGS wave-front sensors • Phasing camera Laser house IFUs in the Era of JWST - October 2010

  10. GMTIFS Summary IFUs in the Era of JWST - October 2010

  11. 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 Physical processes IFUs in the Era of JWST - October 2010

  12. 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 calibration IFUs in the Era of JWST - October 2010

  13. Guide Field Geometry IFUs in the Era of JWST - October 2010

  14. The Formation of Disk Galaxies at High Redshift Science Driver IFUs in the Era of JWST - October 2010

  15. High-z Disk Galaxies NataschaFörster-Schreiber Marie Lemonie-Busserolle Shelley Wright Andy Green Early Bulge Clump Cluster Mature Spiral Flocculent Spiral Elmegreen et al. (2009) IFUs in the Era of JWST - October 2010

  16. Gravitationally Lensed Galaxies MACS J2135-0102, z = 3.075 Tucker Jones Stark et al. 2008, Nature, 455, 775 IFUs in the Era of JWST - October 2010

  17. “AGN” Feedback at High Redshift Science Driver IFUs in the Era of JWST - October 2010

  18. [O III] in Radio Galaxies & ULIRGS Nesvadba 2009; z ~ 2 radio galaxies Alexander et al. 2010; z ~ 2 ULIRG SMM J1237+6203 IFUs in the Era of JWST - October 2010

  19. Massive Nuclear Black Holes Science Driver IFUs in the Era of JWST - October 2010

  20. Nuclear Black Holes Graham (2008) IFUs in the Era of JWST - October 2010

  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 104-106M☼ 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 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

  23. Nuclear Star Clusters 5" Scarlata et al. (2004) IFUs in the Era of JWST - October 2010

  24. Active Galactic Nuclei Science Driver IFUs in the Era of JWST - October 2010

  25. NGC 4151 - Seyfert 1 Galaxy [Fe II] 1.644 μm H2 1-0 S(1) 2.122 μm ThaisaStorchi-Bergmann João Steiner [Ca VIII] 2.321 μm H I Brγ 2.166 μm IFUs in the Era of JWST - October 2010

  26. Protoplanetary Disks and Outflows from Young Stars Science Driver IFUs in the Era of JWST - October 2010

  27. Protostellar Disks and Outflows Tracy Beck IFUs in the Era of JWST - October 2010

  28. 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 • 4 AU resn. with GMT at diffraction limit 100 AU 1 yr at 200 km/s IFUs in the Era of JWST - October 2010

  29. Instrument Design IFUs in the Era of JWST - October 2010

  30. GMTIFS Light Paths AO WFSs GMTIFS IFS NGS WFS F-converters Imager LGS WFS ADC Opt NIR NGS WFS LGS NIR Dichroic Calibration IFUs in the Era of JWST - October 2010

  31. Optics – Trimetric View Spectrograph Tertiary mirror Imager Calibration system IFUs in the Era of JWST - October 2010

  32. First Satisfied Observer! LTAO wave-front sensors GMTIFS cryostat GMTIFS calibration system IFUs in the Era of JWST - October 2010

  33. GMTIFS on Instrument Platform IFUs in the Era of JWST - October 2010

  34. Synergies 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 masvs 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 IFUs in the Era of JWST - October 2010

  36. Continuum Sensitivity: 10:1 in 10,000s AB mag/arcsec2 6 mas; R=10000 6 mas; R=5000 12 mas; R=10000 12 mas; R=5000 25 mas; R=10000 NIFS; R=5000 25 mas; R=5000 JWST; R=2700 50 mas; R=10000 50 mas; R=5000 IFUs in the Era of JWST - October 2010

  37. Line Sensitivity: 200 km/s,10:1 in 10,000s erg/s/cm2/arcsec2 6 mas; R=10000 6 mas; R=5000 12 mas; R=10000 12 mas; R=5000 NIFS; R=5000 25 mas; R=10000 JWST; R=2700 25 mas; R=5000 50 mas; R=10000 50 mas; R=5000 IFUs in the Era of JWST - October 2010

  38. 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

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