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The TMT Instrumentation Program

The TMT Instrumentation Program. Brent Ellerbroek and Luc Simard Pre-SPIE 2010 TMT Instrumentation Workshop San Diego, June 26, 2010. Outline. TMT Instrumentation Program Early Light Instrument Updates WFOS IRIS IRMS First Decade Adaptive Optics Motivations for AO improvements

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The TMT Instrumentation Program

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  1. The TMT Instrumentation Program Brent Ellerbroek and Luc Simard Pre-SPIE 2010 TMT Instrumentation Workshop San Diego, June 26, 2010 TMT.IAO.PRE.10.006.REL01

  2. Outline • TMT Instrumentation Program • Early Light Instrument Updates • WFOS • IRIS • IRMS • First Decade Adaptive Optics • Motivations for AO improvements • First Decade instruments incorporating AO • Facility AO upgrades • Required technology developments • Future Instrumentation Development TMT.IAO.PRE.10.006.REL01

  3. TMT Instrumentation andPerformance Handbook 2010 • 160 pages covering Early-Light and First Decade instrumentation (requirements and designs), instrument synergies, and instrument development • Updated information on early-light instruments • All instrument feasibility studies were combed systematically to extract all available science simulations, and tables of sensitivities/limiting magnitudes/integration times Available at http://www.tmt.org/documents.html TMT.IAO.PRE.10.006.REL01

  4. 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 = 11.2 km • Better Strehl than current AO systems • Can feed three instruments • Completely integrated system • Fast (< 5 min) switch between targets with same instrument • > 50% sky coverage at galactic poles • (WIRC) • NFIRAOS • IRMS • (NIRES) • IRIS TMT.IAO.PRE.10.006.REL01

  5. TMT Science Instrumentation • 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 with the first decade of TMT operations. They include: • Planet Formation Instrument (PFI) • High-Resolution Optical Spectrometer (HROS) • Mid-InfraRed Echelle Spectrometer (MIRES) • InfraRed Multi-Object Spectrometer (IRMOS) • Near-InfraRed Echelle Spectrometer (NIRES) TMT.IAO.PRE.10.006.REL01

  6. Feasibility studies 2005-6 (concepts, requirements, performance,…) IRIS MIRES HROS-UCSC HROS-CASA PFI WFOS-HIA IRMOS-UF IRMOS-CIT

  7. People TMT.IAO.PRE.10.006.REL01

  8. Early Light Instruments TMT.IAO.PRE.10.006.REL01

  9. InfraRed Imaging Spectrometer(IRIS) http://www.tmt.org/docs/WWW_IRIS_DRF01.doc http://irlab.astro.ucla.edu/iris/index.html Also see J. Larkin’s presentation TMT.IAO.PRE.10.006.REL01

  10. IRIS Top-Level Requirements TMT.IAO.PRE.10.006.REL01

  11. Titan with an overlayed 0.05’’ grid (~300 km) (Macintosh et al.) High redshift galaxy. Pixels are 0.04” scale (0.35 kpc). Barczys et al.) M31 Bulge with 0.1” grid (Graham et al.) Keck AO images Motivation for IRIS Unprecedented ability to investigate objects on small scales: 0.01” @ 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)

  12. IRIS Team • James Larkin (UCLA), Principal Investigator • Overall IRIS instrument + lenslet-based IFS • ADC and optical design: UCSC • Anna Moore (Caltech), co-PI • Sharing overall instrument responsibilities + slicer-based IFS • Ryuji Suzuki, Masahiro Konishi, Tomonori Usuda (NAOJ) • Imager design • Betsy Barton (UC Irvine), Project Scientist - Science Team: • Shri Kulkarni (Caltech), Jonathan Tan (U. Florida), Máté Ádámkovics, Joshua Bloom, James Graham, (UC Berkeley), Pat Côté, Tim Davidge (HIA), Shelley Wright (UC Irvine), Bruce Macintosh (LLNL), Miwa Goto (MPIA), Nobunari Kashikawa(NAOJ), Jessica Lu, Andrea Ghez, David Law, Will Clarkson (UCLA), Hajime Sugai (Kyoto) • David Loop, Murray Fletcher, Vlad Reshetov, Jennifer Dunn (HIA) • On-instrument wavefront sensors • Dae-Sik Moon (U. of Toronto): NFIRAOS Science Calibration Unit TMT.IAO.PRE.10.006.REL01

  13. Spectrographs concentric 18” off-axis 2 Coarse Scales (Slicer) 45x90x~2000 elements 1.125”x2.25”@0.025” 2.25”x4.5”@0.050” 2 Fine Scales (Lenslet) 112x128x500 elements 0.45”x0.64”@0.004” 1.0”x1.15”@0.009” Imager Field is on-axis 17” field 0.004” pixels Probe Arms 4” Fields 0.004” pixels Overall Field Geometry • 18” TMT.IAO.PRE.10.006.REL01

  14. Exploded View of IRIS Assembly

  15. On-Instrument Wavefront Sensors NFIRAOS Interface Probe arm Probe Rotational Stage Platform Camera Dewar Probe arm Mature mechanical design ready for probe arm prototyping IRIS Dewar Attachment Thermal Jacket Platform Hexapod Support TMT.IAO.PRE.10.006.REL01

  16. IRIS Science Dewar Entrance Φ = 2m TMT.IAO.PRE.10.006.REL01

  17. Slicer IFU 50mas slicer Camera TMA Slicer collimator Lenslet collimator Grating turret Lenslet 4kx4k spectrograph detector IRIS Imager and Spectrometer Imager channel Schematic view Solid Model TMT.IAO.PRE.10.006.REL01

  18. CFHT/WIRCAM KAB = 24.5 (S/N=5) t = 30 hours !! Point Source Sensitivities • Spectroscopy for S/N per spectral channel of 10, between OH lines, assuming an aperture of 2(λ/D) • Imager for S/N of 100, assuming an aperture of ~2(λ/D) S/N ~10 S/N ~100 Source: S. Wright & B. Barton, 2009

  19. Wide-Field Optical Spectrometer(WFOS) http://www.tmt.org/docs/WWW_WFOS_DRF01.doc Also see B. Bigelow’s presentation

  20. WFOS Top-Level Requirements

  21. WFOS(-MOBIE) Team • Rebecca Bernstein (UCSC), Principal Investigator • Bruce Bigelow (UCSC), Project Manager • Chuck Steidel (Caltech), Project Scientist • 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) • Second feasibility study completed in December 2008 • External review with very positive report • Reflective collimator selected • Conceptual design under way Different WFOS designs were studied during the instrument feasibility study phase. The current design for WFOS is known as the “Multi-Object Broadband Imaging Echellette” (MOBIE) spectrometer.

  22. WFOS-MOBIE Echellette Design Mirror TMT Focal Plane Single field, blue and red arms MOBIE can trade multiplexing for expanded wavelength coverage in its higher dispersion mode Spectral footprint in higher dispersion mode - 3’’ slits spaced 25’’ apart, five orders

  23. WFOS-MOBIE Examples of Spectral Resolution Options TMT.IAO.PRE.10.006.REL01

  24. WFOS-MOBIE Science Field Geometry Source: 2008 WFOS-MOBIE Feasibility Study Operational Concepts Definition Document Multi-object mask making simulation

  25. WFOS-MOBIE Schematic View

  26. InfraRed Multi-slit Spectrometer(IRMS) http://www.tmt.org/docs/WWW_IRMS_DRF01.doc http://irlab.astro.ucla.edu/mosfire/ TMT.IAO.PRE.10.006.REL01

  27. InfraRed Multi-slit Spectrometer (IRMS)(aka Keck/MOSFIRE on TMT)

  28. IRMS and NFIRAOS • 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” • Deployed behind NFIRAOS • 2’ field • 60mas pixels • EE good (80% in K over 30”) • Only one OIWFS required • Spectral resolution up to 5000 • Full Y, J, H, K spectra • Imager as well H-band over whole 120” field Slit width TMT.IAO.PRE.10.006.REL01

  29. Detector area IRMS Slit Unit & Field • 2’ diameter • CSEM configurable slit unit • Slits formed by opposing bars • Up to 46 slitlets • Reconfigurable in ~3 minutes TMT.IAO.PRE.10.006.REL01

  30. “TMT prototype” MOSFIRE integration and test proceeding well MOSFIRE in Caltech Lab

  31. TMT First Decade Adaptive Optics TMT.IAO.PRE.10.006.REL01

  32. Motivations for AO Improvements • New spectral bands • R, I, and Z bands (reduced wavefront error: NFIRAOS+) • L, M, and longer bands not transmitted by NFIRAOS (Mid IR AO -- MIRAO) • Wider fields of view • “Multiplex” observing advantage • Wide field enhanced seeing (Ground Layer AO--GLAO), or… • Moderate field multi-object AO (Multi-Object AO--MOAO) • Higher contrast ratios • Detecting and characterizing planets, other companions (“Extreme” AO--ExAO)

  33. Possible First Decade Instruments Incorporating AO • IR Multi-Object Spectrograph (IRMOS) • MOAO compensation of ~20 integral field units (IFUs) • 5 arc min FoV, 50 mas sampling • ~8 LGS, one order ~60 MEMS for each IFU • 2006 feasibility studies by Caltech and UF/HIA • Pathfinder Multi-Object Spectrograph (PMOS) • A “mini IRMOS” behind NFIRAOS • Perhaps 5 IFUs plus an on-axis imager • NFIRAOS reduces MEMS stroke requirements to < 1 mm • MEMS could also sharpen tip/tilt stars for improved sky coverage • Planet Formation Instrument (PFI) • Contrast ratios in 107-108 range • Order ~128 correction; coronagraphy, advanced WFS detectors/concepts • 2006 feasibility study by LLNL/JPL TMT.IAO.PRE.10.006.REL01

  34. PFI Block Diagram TMT.IAO.PRE.10.006.REL01

  35. IRMOS Block Diagram (UF Concept) MEMS DM NGS WFS LGS WFS TMT.IAO.PRE.10.006.REL01

  36. MOAO Behind NFIRAOS With two DMs, NFIRAOS Strehl and PSF core degrade off-axis at large zenith angles (left) Correction is theoretically much better with MEMS behind NFIRAOS (right) Would benefit both IFUs and natural guide stars Zenith Angle Distance from Center FoV TMT.IAO.PRE.10.006.REL01

  37. Potential Facility AO Upgrades • Mid IR AO facility (MIRAO) • 300-500 nm RMS WFE • Facility system for 2-3 mid IR instruments • Could be an order 30x30 system with 1 DM, 3 LGS • 2006 feasibility study (UH/NOAO) • NFIRAOS upgrade (NFIRAOS+) • ~120 nm RMS WFE for higher Strehls, shorter wavelengths • Could be an order 120x120 upgrade to existing NFIRAOS • Improvements to lasers, DMs, WFSs, and RTC • Ground layer adaptive optics (GLAO) • Enhanced seeing over a wide field of view (e.g., WFOS) • Adaptive secondary mirror required TMT.IAO.PRE.10.006.REL01

  38. MIRAO Optical Schematic Output to Instrument Light from TMT DM LGS WFSs TMT.IAO.PRE.10.006.REL01

  39. AO Component “Desirements” • Higher power lasers • Pulsed format to defeat LGS elongation • IR detectors • Large, high speed, low noise detectors (full frame readout) • Piezo DMs • Order ~120 with large stroke • MEMS DMs • Order 64 to 128 with moderate to large stroke • Adaptive secondary mirror (AM2) • Large, convex, but only ~500 modes of correction required • 2006 feasibility study (SAGEM) • RTCs • Higher throughput and/or more advanced algorithms • Advanced WFSs: Pyramid, post coronagraphic calibration,. … TMT.IAO.PRE.10.006.REL01

  40. Required AO Component Advances by Application TMT.IAO.PRE.10.006.REL01

  41. Future Instrumentation Development TMT.IAO.PRE.10.006.REL01

  42. Defining the TMT Instrumentation Development Program • Observatory Context • Requirements and architectures • Interfaces (optical, mechanical, power and cooling, data and communications) • Common standards and practices • Definition of development and delivery phases • Planning and Management Practices (costing, schedule, risks, etc.) • Development process • Procurement • Participation (TMT partners, broader community) • Support for funding requests • Work package agreements • Models and phasing scenarios TMT.IAO.PRE.10.006.REL01

  43. Defining the TMT Instrumentation Development Program • Instrumentation Development Office • Tasks • Personnel • Development funding • Funding levels • Types of source • Incentives TMT.IAO.PRE.10.006.REL01

  44. Future Instrumentation Development:Proposed Process • Community explorations (scientific and technical) • Consultations (e.g., workshops) • Mini-studies • SAC prioritization • “Cornerstone” of instrumentation development • Well-defined metrics for science, technical readiness, schedule and cost • Balance between AO systems and science instruments • Conceptual Design Studies • Establishment of Board guidelines on scope and cost • Call for Proposals • Study phase (two ~one-year competitive studies for each instrument) • External Reviews • SAC evaluation and recommendations to the Board TMT.IAO.PRE.10.006.REL01

  45. Future Instrumentation Development:Proposed Process (cont.) • Instrumentation contract awards • Observatory (and Board) will negotiate cost and scope of awards considering partnership issues • TMT will provide oversight, monitoring and involvement in all instrumentation projects: • To ensure compatibility with all other Observatory subsystems • To maximize operational efficiency, reliability and minimize cost • To encourage common components and strategies • To ensure that budget and schedules are respected • To manage the development of critical component technologies • This will be the responsibility of an Instrumentation Development Office (IDO) within the Observatory TMT.IAO.PRE.10.006.REL01

  46. Instrumentation Development Office • Joint AO and instrumentation engineering team that provides oversight for all instrumentation activities (except routine support) • Initially primarily occupied with early-light instruments (WFOS, IRIS, IRMS, NFIRAOS) and associated AO systems with increasing shift of effort towards support for future instruments and AO systems • Example: AO group develops AO requirements, leads performance analysis and coordinates/manages all subsystem and component development • Will play a central role within a diverse partnership • Manages and provides systems engineering support (including commissioning) for AO systems and instruments • 4 core FTEs in current operations plan • Instrument development budget of ~$10 M / year TMT.IAO.PRE.10.006.REL01

  47. Building Instrumentation Partnerships • Strong interest from all partners in participating in instrumentation projects: • Primarily driven by science interests of their respective science communities • Large geographical distances and different development models • Broad range of facilities and capabilities • Significant efforts are already under way to fully realize the exciting potential found within the TMT partnership • Goal is to build instrumentation partnerships that make sense scientifically and technically while satisfying partner aspirations TMT.IAO.PRE.10.006.REL01

  48. Acknowledgments The authors gratefully acknowledge 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. TMT.IAO.PRE.10.006.REL01

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