TMT Instrumentation and Performance:

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1 TMT Instrumentation and Performance: A Handbook for the July 2007 TMT Science Workshop May 24, 2007 TMT.INS.PRE REL01 1

2 Important Note Feasibility studies for all TMT instrument concepts were conducted in These studies included more than 2000 pages of scientific and technical information, and this handbook is therefore a highly condensed summary of the planned TMT instrumentation. If the information you require to assess the scientific possibilities of TMT for your research is not found in this Handbook, please do not hesitate to contact the TMT instrumentation group: David Crampton (David.Crampton@nrc-cnrc.gc.ca) Luc Simard (Luc.Simard@nrc-cnrc.gc.ca) Good luck! May 24, 2007 TMT.INS.PRE REL01 2

3 TMT May 24, 2007 TMT.INS.PRE REL01 3

4 TMT Basic Characteristics Collecting area: filled aperture with 30m circumscribed diameter, f/15 Ritchey-Chrétien optical design Wavelength range: µm (goal µm) FOV: 15 diameter (unvignetted), 20 (minimal vignetting) Delivered image quality: Seeing-limited: 80% encircled energy at 0.5 µm = mas including image jitter AO-assisted: 187 nm rms wavefront error on axis over 2 diameter corrected FOV (Current AO systems on 8-10m class telescopes deliver nm rms) May 24, 2007 TMT.INS.PRE REL01 4

5 TMT SAC Instrument Suite May 24, 2007 TMT.INS.PRE REL01 5

6 TMT Discovery Space May 24, 2007 TMT.INS.PRE REL01 6

7 TMT Discovery Space May 24, 2007 TMT.INS.PRE REL01 7

8 TMT Instrumentation TMT instruments are currently divided into two categories: Early Light and First Decade Early light instruments are expected to be available at the start of TMT science operations. This category includes the following instruments: Wide-Field Optical Spectrometer (WFOS) InfraRed Imaging Spectrometer (IRIS) InfraRed Multi-slit Spectrometer (IRMS) First decade instruments are expected to be commissioned within the first decade of TMT operations. They include (in no particular order): Planet Formation Instrument (PFI) High-Resolution Optical Spectrometer (HROS) Mid-InfraRed Echelle Spectrometer (MIRES) InfraRed Multi-Object Spectrometer (IRMOS) Near-InfraRed Echelle Spectrometer (NIRES) May 24, 2007 TMT.INS.PRE REL01 8

9 First Decade Instruments on TMT Nasmyth Platforms May 24, 2007 TMT.INS.PRE REL01 9

10 TMT Adaptive Optics Conventional natural guide star AO: Very limited sky coverage (not enough bright natural stars) Single laser guide star AO: Poor performance due to the cone effect (laser guide star too close to telescope aperture) Laser Tomography AO (LTAO): Multiple laser guidestars used to defeat the cone effect Good AO performance over a narrow field of view Multi-conjugate (and specifically dual-conjugate) AO (MCAO) Multiple (two) deformable mirrors enlarge the corrected field-of view Uniform image quality improves photometry and astrometry Multi-Object AO (MOAO): Separate correction of multiple small objects (like distant galaxies) within a larger field Ground-layer AO (GLAO): Moderately improved seeing over significantly larger fields of view Extreme AO (ExAO): High contrast imaging/spectroscopy May 24, 2007 TMT.INS.PRE REL01 10

11 Mapping AO Modes to Instrumentation Capabilities GLAO 5 MOAO IRMOS WFOS (SRD) FoV Narrow Field NIR ExAO PFI MCAO LTAO MIRES Study? HROS (SRD) High Contrast Diffraction- Limited Enhanced Seeing Seeing- Limited May 24, 2007 TMT.INS.PRE REL01 11 Image Quality

12 Early Light AO Architecture for TMT Supports Narrow-Field Instruments Using Existing/Near-Term Components/Concepts Laser Guide Star Facility 3-6 sodium laser guidestars 3 50W, CW lasers Conventional Secondary LTAO 3 LGS WFS Current piezo DM technology MCAO (NFIRAOS) 6 LGS WFS 2 high-order piezo DMs Mid IR Instruments Narrow-field Near IR May 24, 2007 TMT.INS.PRE REL01 12 Instruments

13 Early Light Instrumentation May 24, 2007 TMT.INS.PRE REL01 13

14 Wide Field Optical Spectrometer (WFOS) Multi-object spectroscopy over two 4.5 x5.4 fields (that extend to 17 diameter at corners) Wavelength range: µm. ADC included Field of view: 46 arcmin 2 ; Total slit length: 650 arcsec Image quality: 0.2 arcsec FWHM over any 0.1µm Spatial sampling: 0.07 arcsec per pixel Spectral resolution: R= for 0.75 slit; goal: WFOS field layout May 24, 2007 TMT.INS.PRE REL01 14 Back to Instrument list

WFOS Science An IGM Tomographic Surveyor Given that TMT will go ~ 2 mag deeper than 8-10m class telescopes, and background UVbright galaxies will become usable beacons, sky surface

15 WFOS Science An IGM Tomographic Surveyor Given that TMT will go ~ 2 mag deeper than 8-10m class telescopes, and background UVbright galaxies will become usable beacons, sky surface density of sightlines will be ~200x higher An individual galaxy halo will therefore be probed through multiple sightlines (R. Cen, Princeton U.) May 24, 2007 TMT.INS.PRE REL01 15

16 WFOS Performance May 24, 2007 TMT.INS.PRE REL01 16

Narrow-Field IR AO System (NFIRAOS): TMT s Early Light Facility AO System Dual conjugate AO system Order 61x61 DM and TTS at h=0 km Order 75x75 DM at h=12 km Better Strehl than current AO systems

17 Narrow-Field IR AO System (NFIRAOS): TMT s Early Light Facility AO System Dual conjugate AO system Order 61x61 DM and TTS at h=0 km Order 75x75 DM at h=12 km Better Strehl than current AO systems Band Strehl Ratio SRD (120 nm) Baseline (177 Baseline + TT nm) R I Z J H K Can feed three instruments Completely integrated system Fast (<5 min) switch between targets with same instrument >50% sky coverage at galactic poles May 24, 2007 TMT.INS.PRE REL01 17

18 InfraRed Imaging Spectrometer (IRIS) An integral field spectrometer and imager working at the diffraction limit: Fed by NFIRAOS (Narrow Field IR AO System) Wavelength range: µm Field of view: < 2 arcsec for IFU, up to 10 for imaging mode Spatial sampling: 4 mas per pixel (Nyquist sampled (λ/2d)) over 4096 pixels for IFU); over 10x10 arcsec for imaging Plate scale adjustable 0.004, 0.009, 0.022, arcsec/pixel 128x128 spatial pixels with small (Δλ/λ 0.05) wavelength coverage Spectral resolution R=4000 over entire J, H, K, L bands, one band at a time R=2-50 for imaging mode Two IFU paths: lenslet-based (for better wavefront quality) and slicerbased (for higher sensitivity) Parallel imaging: goal May 24, 2007 TMT.INS.PRE REL01 18 Back to Instrument list

Motivation for IRIS Should be the most sensitive astronomical IR spectrograph ever built.

05 AU (Nearby stars companions) 100 pc = 1 AU (Nearest star forming regions) 1 kpc = 10 AU (Typical Galactic Objects) 8.

07 kpc (galaxies at solar formation epoch) z=1.0 = 0.

19 Motivation for IRIS Should be the most sensitive astronomical IR spectrograph ever built. Unprecedented ability to investigate objects on small scales. 5 AU = 36 km (Jovian s and moons) 5 pc = 0.05 AU (Nearby stars companions) 100 pc = 1 AU (Nearest star forming regions) 1 kpc = 10 AU (Typical Galactic Objects) 8.5 kpc = 85 AU (Galactic Center or Bulge) 1 Mpc = 0.05 pc (Nearest galaxies) 20 Mpc = 1 pc (Virgo Cluster) z=0.5 = 0.07 kpc (galaxies at solar formation epoch) z=1.0 = 0.09 kpc (disk evolution, drop in SFR) z=2.5 = 0.09 kpc (QSO epoch, Hα in K band) z=5.0 = 0.07 kpc (protogalaxies, QSOs, reionization) Titan with an overlayed May 24, 2007 M31 Bulge 0.05 grid (~300 km) TMT.INS.PRE REL01 with 0.1 grid (Graham et al.) High redshift galaxy. 19 Pixels are 0.04 (Macintosh et al.) Keck AO images scale (0.35 kpc). Barczys et al.)

20 IRIS Concept Imager 4K detector, 15 square field Integral Field Spectroscopy Lenslet option: 128x128 lenses (250 micron pitch) 1000 pixel spectral length (2 pixels per resolution element) Bandpass: 5% per exposure Image Slicer option 88 slices Larger bandpass but poorer wfe Lenslet Array Common reimager camera lens Alternate Gratings On Turret Focal plane layout IRIS will reach point sources as faint as K = 28 (K AB = 30) (3σ) in 3 hours. WIRC precise photometry and astrometry can be done with IRIS but with smaller field Imager Filter Wheels May 24, 2007 TMT.INS.PRE REL01 F/15 AO 20 Focus

21 InfraRed Multi-Slit Spectrometer (IRMS) Clone of Keck MOSFIRE Multi-slit NIR imaging spectro: Step 0 towards IRMOS 46 slits: width 160 mas, length= 2.5 Deployed behind NFIRAOS 2 field Slit width 60 mas pixels Encircled energy (EE) good (80% in K over 30 ) Spectral resolutions up to 5000 Full Y, J, H, K spectra Imager as well Entire NFIRAOS 120 field May 24, 2007 TMT.INS.PRE REL01 21 Back to Instrument list

22 MOSFIRE Concept May 24, 2007 TMT.INS.PRE REL01 22

proposed by HIA (Erickson 2003) Designed for 35K operation Minor mods for

23 IRMS Slit Unit & Field Detector area CSEM configurable slit unit Slits formed by opposing bars Designed for JWST (backup for MEMS shutters) Original concept proposed by HIA (Erickson 2003) Designed for 35K operation Minor mods for MOSFIRE Reconfigurable in ~3 minutes 2 diameter May 24, 2007 TMT.INS.PRE REL01 23

24 IRMS Spectra Full Y, J, H, K spectra with R ~ 5000 with 160mas (2 pix) slits in central ~1/3 of field May 24, 2007 TMT.INS.PRE REL01 24

25 IRMS Performance Encircled energy curves showing the NFIRAOS wide field performance in J, H and K with tomographic reconstructor parameters tuned to optimize image quality over a 30 field (left-hand panels) and a 120 (right-hand panels). The minimum (Nyquist-sampled) IRMS slit width is 160 mas, and it thus encloses light within a radius of 80 mas. May 24, 2007 TMT.INS.PRE REL01 Whole field

26 First Decade Instrumentation May 24, 2007 TMT.INS.PRE REL01 26

27 Planet Formation Instrument (PFI) Wavelength range: 1-2.5µm, goal 1-4µm Field of view 0.7 arcsec radius - goal is 2 arcsec Planet detection contrast 50 mas, goal of 100 mas (5-sigma detection in 2hr integration with I < 8 parent star magnitude) 30 mas, goal of 30 mas (5-sigma detection in 2hr integration with H < 10 parent star magnitude) Critically sampled at H-band ( arcsec pixels), goal is at J- band Spectral resolution, full FOV, IFU: R = 50, goal 100 Spectral resolution, partial FOV, IFU: R = 500, goal 1000 Polarization: simultaneous dual channel May 24, 2007 TMT.INS.PRE REL01 27 Back to Instrument list

28 PFI Science May 24, 2007 TMT.INS.PRE REL01 28 Back to Instrument list

29 PFI Block Diagram May 24, 2007 TMT.INS.PRE REL01 29

30 High Resolution Optical Spectrometer (HROS) Seeing limited optical spectrometer Wavelength range: µm ( µm goal) Field of view: 10 arcsec Image quality: 0.2 arcsec FWHM at detector Total slit length 5 arcsec, separation between orders Spectral resolution: R=50,000 for 1 arcsec slit, R=90,000 with slicer Stability: 1 m/s velocity precision over 10 years Two HROS concepts were competitively studied as part of the TMT instrument feasibility study phase in One concept ( MTHR ) originated from the UC Santa Cruz (PI: S. Vogt), and the other concept ( CU-HROS ) was proposed by a University of Colorado team (PI: C. Froning). May 24, 2007 TMT.INS.PRE REL01 30 Back to Instrument list

31 HROS Science May 24, 2007 TMT.INS.PRE REL01 31 Back to Instrument list

32 HROS MTHR Concept (UCSC) classic echelle design 10m x 11m x 4m 1.6m off-axis parabolic collimators 1.4m camera lenses Echelle: 3x8 mosaic of gratings 1m x 3.5m 8700 pounds May 24, 2007 TMT.INS.PRE REL01 32

33 HROS MTHR Performance May 24, 2007 TMT.INS.PRE REL01 33

34 HROS MTHR Performance May 24, 2007 TMT.INS.PRE REL01 34

35 CU-HROS Concept Completely new concept, using high performance dichroics Transmission of actual Barr filter for ACS is ~95% May 24, 2007 TMT.INS.PRE REL01 35

Dichroic Tree CU-HROS array performance model Net efficiency after 5 reflections/transmissions ranges from 70-77% after degrading predictions to match spec (>95%

36 Dichroic Tree CU-HROS array performance model Net efficiency after 5 reflections/transmissions ranges from 70-77% after degrading predictions to match spec (>95% transmission/reflection) Sharp transition edges (3-5nm) reduce data loss at bin edges High frequency ripples do not line up May 24, 2007 TMT.INS.PRE REL01 36

37 CU-HROS Performance May 24, 2007 TMT.INS.PRE REL01 37

38 Mid-IR Echelle Spectrometer (MIRES) Mid-IR Diffraction Limited Spectrometer, fed by MIRAO (AM2?) 8-18µm, 5-28µm goal Field of view: 10 arcsec Slit length: 3 arcsec sampled at 0.04 arcsec / pixel Spatial sampling 0.017x0.017 arcsec pixels (Nyquist-sampled at 5 µm); 2K detector Spectral resolution 5000< R <100,000 with diffraction-limited slit R=2-50 for imaging mode Thermal background: Should not increase N band background by more than 15% over natural sky + telescope (assuming 5% emissivity at 273K) Sensitivity: Background should be limited by photon statistics in integrations up to 8hrs long May 24, 2007 TMT.INS.PRE REL01 38 Back to Instrument list

39 MIRES Science May 24, 2007 TMT.INS.PRE REL01 39

40 MIRES Concept AURA/NOAO and MIRES UH IfA AO WFS May 24, 2007 TMT.INS.PRE REL01 40

41 Infrared Multi-Object Spectrograph (IRMOS) Deployable IFU spectrometer fed by Multiple Object AO NIR: µm FoV: IFU heads deployable over 5 arcmin field Image quality: diffraction-limited images, tip-tilt arcsec rms Spatial sampling 0.05x0.05 arcsec pixels, each IFU head 2.0 arcsec FOV, 10 IFU units Spectral resolution R= over entire J, H, K bands, one band at a time R=2-50 for imaging mode Two IRMOS concepts were competitively studied as part of the TMT instrument feasibility study phase in One concept ( TiPi ) originated from Caltech (PI: R. Ellis), and the other concept ( UF ) was proposed by a University of Florida team (PI: S. Eikenberry). May 24, 2007 TMT.INS.PRE REL01 41 Back to Instrument list

42 IRMOS Science For studies of galaxy assembly, the power of IRMOS on TMT will transform the z~3 universe into our own backyard May 24, 2007 TMT.INS.PRE REL01 42

TiPi Pickoff Concept Innovative tiled array of mirrors at a relayed, partially compensated focal plane feeds 16 optical trains (with MEMS DMs) to integral

43 TiPi Pickoff Concept Innovative tiled array of mirrors at a relayed, partially compensated focal plane feeds 16 optical trains (with MEMS DMs) to integral field spectrographs Flat 3-axis steering mirrors MEMS-DMs OAPs Tiled MOAO focal-plane 4 of 16 d-ifu spectrograph units May 24, 2007 TMT.INS.PRE REL01 43

44 TiPi Performance May 24, 2007 TMT.INS.PRE REL01 44

45 IRMOS-UF Pickoff Concept Individual probes feed individual spectrographs, each probe contains a miniaturized MOAO system May 24, 2007 TMT.INS.PRE REL01 45

46 IRMOS-UF Performance May 24, 2007 TMT.INS.PRE REL01 46

47 Near IR Echelle Spectrometer (NIRES) Diffraction limited spectroscopy, fed by NFIRAOS Wavelength range: 1-2.4µm Field of view of acquisition camera: 10 arcsec, arcsec/pixel Slit length: 2 arcsec Spatial sampling: Nyquist sampled (λ/2d) Spectral resolution: 20,000<R<100,000 May 24, 2007 TMT.INS.PRE REL01 47 Back to Instrument list

48 NIRES Science Intergalactic medium beyond z = 7 Lyman-alpha systems GRB observations Detailed abundance studies in Local Group stars Chemical evolution in the Galactic Center Chemical evolution in Local group Galaxies Abundance, chemistry and kinematics in star/planet-forming disks Structure and evolution in planet-forming regions of disks Structure and Kinematics of Proto-stellar envelopes Composition of comets Terrestrial planets around low-mass stars and brown dwarfs Characterizing extra-solar planets and brown dwarfs: Probing atmospheres of hot giant and transiting exoplanets Weather on brown dwarfs May 24, 2007 TMT.INS.PRE REL01 48

49 NIRES Concept NIRES could be similar to existing instruments like Keck NIRSPEC May 24, 2007 TMT.INS.PRE REL01 49

50 Wide-field Infrared Camera (WIRC) Precise photometry and astrometry instrument Wavelength range: 0.8-5µm, goal 0.6-5µm Field of view: 30 arcsec, contiguous Image quality: diffraction limited as delivered by AO Spatial sampling: Nyquist sampled (λ/2d) Spectral resolution: R=5-100 with filters Some WIRC science could be done with IRIS May 24, 2007 TMT.INS.PRE REL01 50 Back to Instrument list

TMT Instrumentation Program: Status and Opportunities

TMT Instrumentation Program: Status and Opportunities Luc Simard Science with Giant Telescopes: Public Participation in TMT and GMT Chicago, June 15-18, 2008 June 17, 2008 1 TMT SAC Instrument Suite June