1. GMTIFS – An AO-Corrected Integral-Field Spectrograph and Imager for GMT Peter McGregor The Australian National University 1 IFUs in the Era of JWST - October 2010

2. GIANT MAGELLAN TELESCOPE IFUs in the Era of JWST - October 2010 2

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

4. InstrumentFunction range (microns) Resolving Power FOV GMACSOptical Multi-Object Spectrometer 0.35-1.0250-400064-200 arcmin 2 NIRMOSNear-IR Multi-Object Spectrometer 1.0-2.5Up to ~400049 arcmin 2 G-CLEFOptical High Resolution (Doppler) Spectrometer 0.4-0.7150K7 x 1” fibers GMTNIRSNear-IR High-Resolution Spectrometer 1.2- 5.025K-100KSingle object GMTIFSNIR AO-fed IFU+Imager0.9-2.55000-10000<5” TIGERMid-IR Imaging Spectrometer 3.0-25.0150030” IFUs in the Era of JWST - October 2010 4 GMT First-Light Instrument Studies Wide-field instruments LTAO instruments

5. Timeline Sept 2011: Six Conceptual Design Reviews Oct 2011: Down select to 2-3 first-light instruments 2020: GMT first light IFUs in the Era of JWST - October 2010 5 What will we want to be doing in 10 yr time?

6. LASER TOMOGRAPHY ADAPTIVE OPTICS IFUs in the Era of JWST - October 2010 6

7. 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

8. 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

9. IFUs in the Era of JWST - October 2010 9 LTAO System Layout LGS 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

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

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

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 12 Spaxel size (mas)6122550 Field of view (arcsec)0.54×0.271.08×0.542.25×1.134.5×2.25

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

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

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

16. 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

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

18. [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

19. SCIENCE DRIVER Massive Nuclear Black Holes IFUs in the Era of JWST - October 2010 19

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

21. 21 Nuclear Black Holes High spatial resolution is required at high-mass end R = GM BH /σ 2 ~ 10.8 pc (M BH /10 8 M ☼ )(σ/200 km/s) -2 ~ 35.3 pc (M BH /10 9 M ☼ )(σ/350 km/s) -2 H-band diffraction limit ~ 16 mas 10 pc @ z = 0.04 35 pc @ z = 0.15 > 5×10 9 M ☼ can be resolved at any distance High spectral resolution is required at low-mass end Probe 10 4 -10 6 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. 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 IFUs in the Era of JWST - October 2010 23 Scarlata et al. (2004) 5"5"

24. SCIENCE DRIVER Active Galactic Nuclei IFUs in the Era of JWST - October 2010 24

25. NGC 4151 - Seyfert 1 Galaxy IFUs in the Era of JWST - October 2010 25 [Fe II] 1.644 μm H 2 1-0 S(1) 2.122 μm H I Brγ 2.166 μm [Ca VIII] 2.321 μm Thaisa Storchi-Bergmann João Steiner

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

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

28. 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

29. INSTRUMENT DESIGN IFUs in the Era of JWST - October 2010 29

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

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

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

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

34. SYNERGIES IFUs in the Era of JWST - October 2010 34

35. 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

36. 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=10000 25 mas; R=5000 50 mas; R=10000 50 mas; R=5000 JWST; R=2700 AB mag/arcsec 2 NIFS; R=5000

37. 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=10000 6 mas; R=5000 12 mas; R=10000 12 mas; R=5000 25 mas; R=10000 25 mas; R=5000 50 mas; R=10000 50 mas; R=5000 erg/s/cm 2 /arcsec 2 NIFS; R=5000

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 38