TMT Instrumentation Program: Status and Opportunities

Transcription

1 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,

2 TMT SAC Instrument Suite June 17,

3 TMT SAC Instrument Suite Visible, Seeing-Limited June 17,

4 TMT SAC Instrument Suite Near-IR, AO-assisted June 17,

5 TMT SAC Instrument Suite High-Contrast AO June 17,

6 TMT SAC Instrument Suite Mid-infrared, AO-assisted June 17,

7 TMT Aperture Advantage with Adaptive Optics Seeing-limited observations and observations of resolved sources Sensitivity ηd 2 (~ 14 8m) Background-limited AO observations of unresolved sources Sensitivity ηs 2 D 4 (~ 200 8m) High-contrast AO observations of unresolved sources Sensitivity η S2 1 S D4 (~ 200 8m) High-contrast ExAO observations of unresolved sources Contrast D 2 (~ 14 8m) Sensitivity ηd 6 (~ m) Sensitivity =1/ time required to reach a given s/n ratio η = throughput, S = Strehl ratio. D = aperture diameter June 17,

8 Feasibility Study Phase - Request For Proposals Announcement of Opportunities sent in January 2005 to institutions across North America - 40 responses leading to 15 proposals The proposals were reviewed by panels mostly composed of external referees plus a SAC member Several collaborative studies emerged: IRIS (UCLA and Caltech) MIRES (NOAO and U Hawaii) (plus supporting MIRAO study) NIRES (UH and NOAO) WFOS (HIA) and a costing study of Caltech MILES design (plus GLAO studies) PFI (LLNL, JPL, U de Montreal) Studies of two different concepts for two of the instruments: HROS: UCSC and U Colorado IRMOS: U Florida and Caltech (plus supporting MOAO study at CfAO) Contracts and work packages were negotiated with all 14 groups ~$1.6M total budget TMT funds were considerably leveraged, especially by some teams. June 17,

9 Feasibility studies (concepts, requirements, performance, ) IRIS MIRES HROSUCSC HROSCASA PFI 9 WFOS-HIA IRMOS-UF IRMOS-CIT

10 Results of Feasibility Study Phase ~200 scientists and engineers involved; at 34 US institutions, 10 Canadian, 2 French institutions VERY successful - Excellent reports on all instrument studies: Extended science cases (with detailed simulations) Technical design + functional/performance requirements documents Observing program definitions (--> Design Reference Mission) 35 external reviewers, mostly instrument experts from 8-10m class telescopes, reviewed the studies. Reviewers brought external perspectives, different experiences Very useful on-line discussions preceded face-to-face reviews Face-to-face meetings between panels and teams took place in March 2006 Excellent review panel reports Lots of advice about potential issues related to aggressive requirements, schedule, complexity, instrument priorities, etc. June 17,

11 From Science to Instrument Concepts: WFOS Observing Programs June 17,

12 Nasmyth Configuration: First Decade Instrument Suite

13 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 (WIRC) Band Strehl Ratio SRD (120 nm) Baseline (177 Baseline + TT nm) R I Z J H K IRMS (NIRES) IRIS NFIRAOS Can feed three instruments Completely integrated system Fast (< 5 min) switch between targets with same instrument > 50% sky coverage at galactic poles June 17,

14 Impact of Feasibility Study Phase Results on TMT Systems Choice of early-light instruments by TMT SAC (incl. US community members) with workhorse scientific capabilities and synergy with ALMA and JWST: IRIS WFOS IRMS Instrument Systems Target acquisition sequences Access and servicing Observatory is being designed as an end-to-end system to maximize performance in diffraction-limited regime Observatory systems Nasmyth platforms (e.g., mass budget, area, height, M1 airflow) Cooling systems (e.g., vibrations must be minimized) Cranes June 17,

15 Infrared Imaging Spectrograph (IRIS) Integral Field Spectrograph and Imager working at the diffraction limit Fed by NFIRAOS (Narrow field facility AO System) Wavelength range: µm; goal 0.6-5µm 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 Parallel imaging: goal June 17,

16 IRIS Team James Larkin (UCLA), Principal Investigator Overall IRIS instrument (including WFS, cal, etc) Lenslet-based IFS ADC and optical design: UCSC Anna Moore (Caltech), co-i Sharing overall instrument responsibilities Slicer-based IFS Tomonori Usuda and IRIS-Japan team Imager design Betsy Barton (UC Irvine), Project Scientist Science Team Pat Cote (HIA), Andrea Ghez (UCLA), Shri Kulkarni (Caltech), David Law (Caltech), Jonathan Tan (U. Florida), Joshua Bloom (UC Berkeley), Tim Davidge (HIA), Shelley Wright (UCLA) June 17,

17 IRIS NFIRAOS Enclosure (at -30C) Interface/WFS unit IRIS IFUs (2 x 2 ) IRIS imager (15 x15 ) IR TT(F) Wavefront Sensors (5 x 5 ) Imager Filter Wheels ADC for Visible imager?? F/15 AO Focus IRIS dewar (at 77k) Lenslet Array Grating Basically 3 instruments: Lenslet IFU Slicer IFU Imager June 17,

18 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 0.05 grid (~300 km) (Macintosh et al.) M31 Bulge with 0.1 grid (Graham et al.) Keck AO images 18 High redshift galaxy. Pixels are 0.04 scale (0.35 kpc). Barczys et al.)

19 Wide Field Optical Spectrometer (WFOS) June 17,

20 WFOS(-MOBIE) Team Rebecca Bernstein (UCSC), Principal Investigator Bruce Bigelow (UCSC), Project Manager Chuck Steidel (Caltech), Project Scientist Discussions of Japanese collaboration under way Science Team Bob Abraham (U. Toronto), Jarle Brinchmann (Leiden), Judy Cohen (Caltech), Sandy Faber, Raja Guhathakurta, Jason Kalirai, Jason Prochaska, Connie Rockosi (UCSC), Gerry Lupino (UH IfA), Alice Shapley (UCLA) First phase of new concept study to be completed by September Conceptual design complete by mid 2009 June 17,

21 WFOS-MOBIE Echellette Design MOBIE can trade multiplexing for expanded wavelength coverage in its higher dispersion mode Bernstein et al. 2008, SPIE 2008 Spectral footprint in higher dispersion mode - 3 slits spaced 25 apart, five orders June 17,

22 IGM Tomography with WFOS Given that TMT+WFOS will go ~ 2.5 mag deeper than 8-10m class telescopes, and background UV-bright galaxies will then become usable beacons, the surface density of sightlines on the sky for intergalactic medium tomography will be ~200x higher. This means that one will be able to probe individual galaxy haloes through multiple sightlines. (R. Cen, Princeton U.) June 17,

23 InfraRed Multi-slit Spectrometer (IRMS - Keck/MOSFIRE on TMT) IRMOS (deployable MOAO IFUs) deemed too risky and too expensive for first light => IRMS: clone of Keck MOSFIRE; Step 0 towards IRMOS Multi-slit NIR imaging spectro: 46 slits,w:160+ mas, L:2.5 Slit width Deployed behind NFIRAOS 2 field 60mas pixels EE good (80% in K over 30 ) Spectral resolution up to 5000 Full Y, J, H, K spectra Imager as well Whole 120 field June 17,

24 IRMS Spectra Full Y, J, H, K spectra with R ~ 5000 with 160mas (2 pix) slits in central ~1/3 of field June 17,

25 Instrument Systems: LGS IRIS Acquisition Sequence LGS IRIS, IFU mode Baseline acquisition scenario using the acquisition camera: 289 s (~4.8 minutes)* Alternative scenarios: - Blind acquisition scenario: 219 s (~3.6 minutes)* -Spiral acquisition scenario: 224 s (~3.7 minutes after 2 steps)* *assuming 3 minutes for telescope setup June 17,

26 Instrument Systems: Access and Servicing June 17,

27 Observatory Systems: Cooling R507-coolant circuit for NFIRAOS (Similar circuits to be used for instrument electronics enclosures) Two-stage, closed loop, gaseous helium system for cryogenic instruments - eliminates vibrations on Nasmyth platforms June 17,

28 Future Plans and Opportunities Conceptual studies are currently underway for IRIS and WFOS (~ $700K each). Opportunities for involvement in the TMT early-light instruments are always available to potential partners, e.g., Japanese involvement in IRIS (TMT s top priority instrument). Future development efforts will be patterned after our highly successful instrument feasibility phase: Request for proposals issued to the broad community Competitive studies Extensive external reviews Plans are to bring five additional instruments on-line within the first decade of TMT operations $15M/yr instrument budget According to the TMT funding-paced schedule, calls for proposals will be issued at the start of construction June 17,

29 TMT Foundation Documents Detailed Science Case 2007 Observatory Requirements Document Observatory Architecture Document Operations Concept Document TMT Construction Proposal Currently in use for funding proposals June 17,

30 Acknowledgments The TMT Project gratefully acknowledges the support of the TMT partner institutions. They are the Association of Canadian Universities for Research in Astronomy (ACURA), the California Institute of Technology and the University of California. This work was supported as well by the Gordon and Betty Moore Foundation, the Canada Foundation for Innovation, the Ontario Ministry of Research and Innovation, the National Research Council of Canada, the Natural Sciences and Engineering Research Council of Canada, the British Columbia Knowledge Development Fund, the Association of Universities for Research in Astronomy (AURA) and the U.S. National Science Foundation. June 17,