1. The TMT Instrumentation Program David Crampton Meeting with Chinese Delegation Pasadena June 4, 2009 (crampton@tmt.org)

2. October 4, 2015 TMT.IAO.PRE.09.035.REL01 2 Outline Philosophy and goals for TMT instrumentation –Instrumentation includes Science Instruments and AO Intro and brief history –Feasibility studies 2005-6 Current status –Conceptual design studies for early light instrument Future instrumentation development

3. October 4, 2015 TMT.IAO.PRE.09.035.REL01 3 Key Requirement: to realize the full scientific potential of a diffraction-limited 30m telescope

4. October 4, 2015 TMT.IAO.PRE.09.035.REL01 4 Goals for Instrumentation Program Maximize scientific output –Input: extensive discussions about scientific priorities with SAC, feasibility studies, community meetings (e.g. Irvine ELT Science meeting, 2007) –Attempt to pace the design and development effort to take advantage of latest innovations –Maintain versatility and options Deliver cost effective state-of-the-art instruments for first light Ensure that entire Observatory system is optimized to produce the best possible science Establish telescope and observatory requirements and interfaces for instruments of all types Establish costs and schedules Understand risks and mitigation strategies Develop plans for ongoing instrument development

5. October 4, 2015 TMT.IAO.PRE.09.035.REL01 5 Instrumentation Philosophy Using world-class teams, develop best possible instrument concepts to meet the scientific requirements –Attempt to engage whole astronomical community, including international partnerships Plan to utilize (and help sustain) partnership expertise and experience –Build on successful Keck model for instruments (instrument teams stay involved) Keep TMT instrumentation development staff to a minimum –Fully utilize partners and wider community –Minimal in-house development

6. October 4, 2015 TMT.IAO.PRE.09.035.REL01 6 Capability Spectral Resolution Science Case Near-IR DL Spectrometer & Imager (IRIS) ≤4000 Assembly of galaxies at large redshift Black holes/AGN/Galactic Center Resolved stellar populations in crowded fields Astrometry Wide-field Optical Spectrometer (WFOS) 300 - 5000 IGM structure and composition 2<z<6 High-quality spectra of z>1.5 galaxies suitable for measuring stellar pops, chemistry, energetics Multi-IFU, near-DL, near- IR Spectrometer (IRMOS) 2000 - 10000 Near-IR spectroscopic diagnostics of the faintest objects JWST followup Mid-IR Echelle Spectrometer & Imager (MIRES) 5000 - 100000 Physical structure and kinematics of protostellar envelopes Physical diagnostics of circumstellar/protoplanetary disks: where and when planets form during the accretion phase ExAO I (PFI) 50 - 300 Direct detection and spectroscopic characterization of extra-solar planets High Resolution Optical Spectrograph (HROS) 30000 - 50000 Stellar abundance studies throughout the Local Group ISM abundances/kinematics, IGM characterization to z~6 Extra-solar planets! MCAO imager (WIRC) 5 - 100 Galactic center astrometry Stellar populations to 10Mpc Near-IR, DL Echelle (NIRES) 5000 - 30000 Precision radial velocities of M-stars and detection of low-mass planets IGM characterizations for z>5.5 Science Flowdown => SRD Instrument Suite

7. October 4, 2015 TMT.IAO.PRE.09.035.REL01 7 Instruments are all located on two large Nasmyth structures HROS WFOS IRMOS MIRAO/ MIRES APS PFI NFIRAOS IRIS (bottom port) WIRC NIRES-B

8. October 4, 2015 TMT.IAO.PRE.09.035.REL01 8 NFIRAOS feeds 3 instruments Dual conjugate AO system – Better Strehl and larger field than current systems (despite being harder for a 30m!) Completely integrated system Fast (<5 min) switch between targets High sky coverage, even at galactic poles VLT/MAD results demonstrate MCAO potential NFIRAOS IRIS ( WIRC ) IRMS (NIRES)

9. October 4, 2015 TMT.IAO.PRE.09.035.REL01 9 TMT Instrument Feasibility Studies 2005-6 An Announcement of Opportunity for feasibility studies for 8 instruments and conceptual design for NFIRAOS was issued widely to potential institutions across North America in early 2005 Feasibility studies launched in Apr 2005; reviewed in Mar 2006 –IRIS (UCLA and Caltech) –MIRES (NOAO and U Hawaii) + NIRES mini-study –WFOS (HIA) and GLAO plus a “MILES costing study” at Caltech –PFI (LLNL, JPL, U de Montreal) –HROS: 2 studies - UCSC and U Colorado –IRMOS: 2 studies - U Florida and Caltech plus MOAO at UCSC –Major collaborations formed –~200 scientists and engineers involved; at 34 US institutions, 10 Canadian, 2 French institutions –Reviewed by panels of international experts (35 reviewers) => Produced performance, cost and schedule estimates for feasible instruments, requirements for the telescope system, identified risks, developed concepts for operation

10. October 4, 2015 TMT.IAO.PRE.09.035.REL01 10 Feasibility studies 2005-6 (concepts, requirements, performance,…) HROS-CASA IRMOS-UFWFOS-HIA HROS-UCSC MIRES IRMOS-CIT IRIS PFI

11. October 4, 2015 TMT.IAO.PRE.09.035.REL01 11 Feasibility studies 2005-6 (concepts, requirements, performance,…) HROS-CASA IRMOS-UFWFOS-HIA HROS-UCSC MIRES IRMOS-CIT IRIS PFI The SRD instrument suite is likely to be representative of TMT instruments Seeing-limited and diffraction-limited UV to MIR High Contrast imaging All field sizes up to 20 arcmin => It should be appropriate for defining global instrument requirements => It should provide flexibility for future instruments to respond to science that can’t yet be foreseen.

12. October 4, 2015 TMT.IAO.PRE.09.035.REL01 12 Overall Conclusions from feasibility studies 30m instruments are challenging but feasible –Some require up to ~10 years and some cost >$60M Some examples –HROS: High Resolution Optical Spectrometer Spectral resolution: R=50,000 for 1” slit, R=90,000 with slicer => Characteristic size 10m, large optics, cost up to $50M –IRMOS: NIR deployable IFU spectrometer fed by MOAO >10 IFU over 5’ field of regard => Complex, MOAO not mature, cost up to $75M (for 20 dIFU) –NIRES: Diffraction-limited NIR Echelle Spectrometer 20,000 < R < 100,000 => Straightforward, cost ~$11M Total cost ($2006 base year) of SRD instruments (no contingency, no AM2), based on estimates from feasibility studies ~$223M + supporting AO systems ~$57M, i.e., > $280M

13. October 4, 2015 TMT.IAO.PRE.09.035.REL01 13 Early Light Instrument suite established in late 2006 Instrument priorities set by SAC (incl. US community members): “ Workhorse ” scientific capabilities, synergy with JWST and ALMA –IRIS (Infrared Imager and Integral Field Spectrograph) –WFOS (Wide Field multiobject Optical Spectrograph –IRMS (Infrared Multi-slit Spectrograph and imager) Excellent science –Exploits huge gains in wide range of science at the NIR diffraction limit –Good balance of capabilities for “flagship” science as well significant “discovery” potential –Broad range of science enabled Good early light suite –Broad range of wavelengths, spectral and spatial resolution –Seeing-limited and diffraction-limited –All three are modest extrapolations of current 8-10m instruments –Relatively simple to quickly commission –Will provide excellent PR!

14. October 4, 2015 TMT.IAO.PRE.09.035.REL01 14 Early Light Instrument teams (Aug 2007 announcement) “Goal is to form strong teams, mostly from within TMT partnership, that will be able to deliver the best possible instruments that meet the science requirements, on schedule and within budget” “Strong science teams will be essential for success of instruments –Develop detailed requirements, provide simulations of performance, examine tradeoffs, assist in testing, identify commissioning targets, determine optimal observing strategies, participate in early light observations, publish first data” “Broad representation of TMT science and partners desired” => Conceptual designs for the first light instruments are in progress –Future instruments will be started in ~2013, subject to availability of development funds. These are expected to be competed and open to the broader community. Teams for these instruments are mostly already formed, although additions to teams and other contributions are welcome, especially in certain areas.

15. October 4, 2015 TMT.IAO.PRE.09.035.REL01 15 IRIS Conceptual Design Team James Larkin (UCLA), PI, Lenslet IFS Anna Moore (Caltech), co-I, Slicer IFS Ryuji Suzuki, Masahiro Konishi, Tomonori Usuda (NAOJ), Imager Betsy Barton (UC Irvine), Project Scientist Science Team – Mate Adamkovics(UCB), Aaron Barth(UCI), Josh Bloom(UCB), Will Clarkson(UCLA), Pat Cote(HIA), Tim Davidge(HIA), Andrea Ghez(UCLA), Miwa Goto(MPIA), James Graham(UCB), Nobunari Kashikawa(Subaru), Shri Kulkarni(Caltech), David Law(UCLA), Jessica Lu(UCLA), Bruce Macintosh(LLNL), Hajime Sugai(Kyoto U), Jonathan Tan(UF), Tomonori Usuda(NAOJ), Shelley Wright(UCI) OIWFS ( On Instrument Wavefront Sensor ) Team (HIA + Caltech) –Led by David Loop, Anna Moore NSCU ( NFIRAOS Science Calibration Unit ) Team (U of Toronto) –Led by Dae-Sik Moon Design proceeding well; interim review earlier this week

16. October 4, 2015 TMT.IAO.PRE.09.035.REL01 16 Motivation for IRIS Should be the most sensitive astronomical IR spectrograph ever built 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, H  in K band) z=5.0= 0.07 kpc(protogalaxies, QSOs, reionization) 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

17. October 4, 2015 TMT.IAO.PRE.09.035.REL01 17 IRIS: Diffraction Limited Imager, Slicer and Lenslet Integral Field Spectrograph Imager 17”x17”, 4 mas pixels –Precision photometry –30microarcsec relative astrometry Lenslet Integral field Spectrograph –128 x 128 lenses –Bandpass: 5%/exposure –Finest scales (4, 9 mas), best wfe Slicer IFS –45 slices, field up to 2”x4” –25, 50 mas scales –Best sensitivity IFSs share camera and detector NFIRAOS MCAO system (Enclosure at -30C) ImagerLenslet and slicer foreoptics Common camera and detector

18. October 4, 2015 TMT.IAO.PRE.09.035.REL01 18 WFOS Team Rebecca Bernstein (UCSC), PI Bruce Bigelow (UCSC), PM Chuck Steidel (Caltech), PS Science Team: Bob Abraham(U Toronto), Jarle Brinchmann(Leiden), Judy Cohen(Caltech), Sandy Faber(UCSC), Raja Guhathakurta(UCSC), Jason Kalirai(UCSC), Gerry Lupino(UH), Jason Prochaska(UCSC), Connie Rockosi(UCSC), Alice Shapley(UCLA) Some “flagship” science cases, “work horse capability” –High quality spectra of faint galaxies/AGN/stars –IGM tomography Great “follow-up” and “discovery” potential - full wavelength coverage with spectral resolutions up to R = 8000 –JWST, ALMA, etc., follow-up Sensitivity >14 x current 8m telescopes New feasibility study completed; conceptual design just starting.

19. October 4, 2015 TMT.IAO.PRE.09.035.REL01 19 WFOS-MOBIE Seeing-limited, 0.3-1mu Probably only optical capability for ~ first 5 years –“Discovery”, “Diagnostic” and survey science Echellette design –Full wavelength coverage Blue and Red channels –Multi-object –R ~1000 - 8000 –9’ x 4’ field Simple single barrel design –300mm pupils –Fixed dichroic beamsplitter Up to 5 orders at highest R Reflecting collimator, refractive camera Prism cross dispersion

20. October 4, 2015 TMT.IAO.PRE.09.035.REL01 20

21. October 4, 2015 TMT.IAO.PRE.09.035.REL01 21 IR Multi-Slit Spectrometer (IRMS) IRMOS (deployable MOAO IFUs) deemed too risky/expensive for first light => IRMS: clone of Keck MOSFIRE, first step 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”) –Spectral resolution up to 5000 –Full Y, J, H, K spectra (one at a time) Images entire 2’ field Slit width Whole 120” field

22. October 4, 2015 TMT.IAO.PRE.09.035.REL01 22 IRMS Spectra Configurable Slit Unit originally developed for JWST (slits formed by opposing bars) Full Y, J, H, K spectra with R ~ 5000 with 160mas (2 pix) slits in central ~1/3 of field

23. October 4, 2015 TMT.IAO.PRE.09.035.REL01 23 IRMS Spectra Configurable Slit Unit originally developed for JWST (slits formed by opposing bars) Full Y, J, H, K spectra with R ~ 5000 with 160mas (2 pix) slits in central ~1/3 of field

24. October 4, 2015 TMT.IAO.PRE.09.035.REL01 24 MOSFIRE in Caltech Lab “TMT prototype” MOSFIRE integration and test proceeding well

25. October 4, 2015 TMT.IAO.PRE.09.035.REL01 25 A Key IRMS Project: Exploring the Early Universe Early Sources and cosmic reionization –Synergy with JWST and 21cm surveys: Expect JWST to detect brightest sources in each ionized bubble. TMT, with AO, should go 1 mag fainter (or more if objects are physically small) TMT IRIS, IRMS and NIRES will study detailed properties of first galaxies and influence on IGM –Pop III stars (intense HeII 1640) –Tracing SF (Ly Alpha) in ionized bubbles –Escape fraction from Ly alpha profiles –IGM at z > 7 using quasars or GRBs Unlensed sizes ~30mas IRMS science team now being formed, led by Bahram Mobasher (UCR)

26. October 4, 2015 TMT.IAO.PRE.09.035.REL01 26 Efficient Operation: Observation Workflow Target acquisition –< 5 minutes including slewing, configuring, finding target, setting up AO system Instrument changes –< 10minutes to opening shutter Example: Part of IRIS LGS sequence (40 subtasks)

27. October 4, 2015 TMT.IAO.PRE.09.035.REL01 27 Efficient Operation: Observation Workflow Target acquisition –< 5 minutes including slewing, configuring, finding target, setting up AO system Instrument changes –< 10minutes to opening shutter Example: Part of IRIS LGS sequence (40 subtasks) Studied extensively - Vital input to requirements of all observatory subsystems - Report available “Observation Workflow for TMT” TMT.AOS.TEC.07.013 VERY Challenging but both key timing requirements appear feasible

28. October 4, 2015 TMT.IAO.PRE.09.035.REL01 28 Rapid Response Example: GRBs and TMT GRBs are very bright but only briefly Expect a significant fraction at very high redshift GRBs are point sources - D 4 advantage with AO => Potential for high S/N, high resolution spectra –Physics of extreme events and objects at high z –IGM studies at high z Instruments: –WFOS measurements of redshift, physical conditions –IRIS imaging and IFS with R = 4000 Detection and IFU spectroscopy of host galaxies –NIRES (AO fed) R = 50,000 spectroscopy over 0.8 - 2.5mu Time sequences of high S/N spectra of high z objects –MIRES: R = 100,000 spectroscopy in 5-28micron region –HROS: R = 50,000 spectroscopy in 0.3 - 1micron region GRB090423

29. October 4, 2015 TMT.IAO.PRE.09.035.REL01 29 Development of Future Instruments

30. October 4, 2015 TMT.IAO.PRE.09.035.REL01 30 Objectives Capabilities similar to the first decade suite are required to fulfill TMT science requirements –Community will want additional capabilities ASAP Upgrade to an adaptive secondary (AM2) will globally improve performance and simplify some systems Upgrade NFIRAOS to 130nm WFE as per SRD (high strehl in J band) will improve performance Maintain TMT at forefront of international astronomical research Teams for these instruments are completely open

31. October 4, 2015 TMT.IAO.PRE.09.035.REL01 31 Example of Future Instruments: HROS UCSC Concept 12m * 16m * 4m! PI: Vogt Co-I: Rockosi Classic echelle –12m * 16m –3m off-axis parabolic collimators –1.3m camera lenses –Huge echelle 5x8 mosaic of gratings 1m x 3.5m

32. October 4, 2015 TMT.IAO.PRE.09.035.REL01 32 Completely new concept, using high performance dichroics (PI: Froning) Transmission of actual Barr filter for ACS is ~95% Example of Future Instruments: HROS CASA Concept

33. October 4, 2015 TMT.IAO.PRE.09.035.REL01 33 HROS Science Cases Detailed abundance measurements for stars as faint as V~20. Abundance measurements will be made for main-sequence stars in nearby globular clusters, large samples of giant stars throughout the Galactic halo and bulge and samples of giant stars in galaxies throughout the Local Group. Doppler-based searches for extra-solar planets. The existing searches for extra- solar planets based on measuring extremely precise (  < 2 m/sec) will be extended to lower-mass (and statistically fainter) stars and therefore be sensitive to lower- mass planets. With increased S/N, detailed line-shape analysis will also make it possible to further increase the velocity precision of the measurements and push to smaller planet masses. Abundances, kinematics and physical conditions in the inter-galactic medium to z~7. Absorption-line studies using QSOs with I≤20 will provide measurements of element abundances in the IGM throughout most of the history of the Universe. Gas kinematics, physical conditions and the correlation functions in 3-D will be possible over a large range in z.

34. October 4, 2015 TMT.IAO.PRE.09.035.REL01 34 Detection of Habitable Terrestrial Planets Around Nearby G,K,M Stars Gliese 876 M4V at 15pc A 7.5 earth-mass rock… 5 M Earth habitable zone planet detected in 50 observations spread over 150 nights with TMT/MTHR 60-d 30-d 1.9-d GJ 876d Planet Detectability at 15 pc

35. October 4, 2015 TMT.IAO.PRE.09.035.REL01 35 TMT Solar System Capabilities Spatial resolution (25km at Jupiter) comparable to fly-by space probes (at least in outer solar system) Spectral resolution (0.3 - 30micron) >> space probes Sensitivity ~ JWST, ALMA Good temporal monitoring possible to observe variable phenomena (atmosphere and surface) Short time scale to respond to transient and unpredictable events Precision (< 100 microarcsec) astrometry Precision (< m/s) radial velocities

36. October 4, 2015 TMT.IAO.PRE.09.035.REL01 36 TMT Solar System Capabilities Spatial resolution (25km at Jupiter) comparable to space probes (at least in outer solar system) Spectral resolution (0.3 - 30micron) >> space probes Sensitivity ~ JWST, ALMA Good temporal monitoring possible to observe variable phenomena (atmosphere and surface) Short time scale to respond to transient and unpredictable events Precision (< 100 microarcsec) astrometry Precision (< m/s) radial velocities Small community at present but a lot of public interest: 2% of HST time spent on solar system => 1/3 of press!

37. October 4, 2015 TMT.IAO.PRE.09.035.REL01 37 Guidelines for Future Instruments Instrument development should be competitive –Caveat: subject to funding, partnership agreements, etc –Will attempt to involve broad community in projects (at a minimum, on the science teams). IRIS is a good example of this. TMT will provide oversight, monitoring and involvement in all instruments –To ensure compatibility with overall system –To maximize operational efficiency, reliability and minimize cost –To encourage common components and strategies –To ensure that budget and schedules are respected Priorities expected to be updated every few years by SAC Cycle time is typically 8-9 years from initial RFP to end of technical commissioning (although only 5-6 years to “build”).  Must start successive instruments soon after construction start

38. October 4, 2015 TMT.IAO.PRE.09.035.REL01 38 Typical Development Cycle (2 instruments, one simple, one complex) 201120122013201420152016201720182019202020212022 Conceptual Design Phase (competitive) Design and build instrument 1 Construction start Choose 2 new Instruments for study BOD decision (scope, funding cap, partner issues) Design and build instrument 2 First Light Conceptual Design Phase (competitive) Commission

39. October 4, 2015 TMT.IAO.PRE.09.035.REL01 39 Cartoon of development funding profile (Fiscal Years, $M2009) Instruments are commissioned in the blue-filled cells.

40. October 4, 2015 TMT.IAO.PRE.09.035.REL01 40 Instrument Development Office Joint AO and INST engineering team that provides oversight for all instrumentation development activities (except routine support) –Initially primarily occupied with WFOS, IRIS, IRMS, NFIRAOS and associated AO systems (Construction budget) –Increasing shift of effort towards support for future instruments and AO systems (DEV budget) –E.g., AO group develops AO requirements, leads performance analysis, and coordinates/manages all subsystem and component development Manages and provides systems engineering support (including commissioning) for AO systems and instruments –~5 projects at any given time 11 FTEs, most likely based in N. America (or Hawaii)

41. October 4, 2015 TMT.IAO.PRE.09.035.REL01 41 SUMMARY Three powerful “workhorse” instruments are being developed, ready for first light in 2018 Next instruments should be commenced immediately after construction starts –To be ready for science starting ~3 yr after first light Funding must ramp up to ~$20M per yr by ~FY2018 Additional funding required to deliver the most challenging instruments and their AO systems in a timely fashion

42. October 4, 2015 TMT.IAO.PRE.09.035.REL01 42 HROS, NIRES, WFOS IRIS, IRMOS PFI MIRES NIRES HROS IRIS WFOS IRIS IRMOS

43. October 4, 2015 TMT.IAO.PRE.09.035.REL01 43 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.

44. October 4, 2015 TMT.IAO.PRE.09.035.REL01 44 NFIRAOS+LGSF+IRIS 2018: Ready for first AO light

45. October 4, 2015 TMT.IAO.PRE.09.035.REL01 45 Angular Sizes and Synergy with JWST Complimentary –JWST has greater sensitivity for z > 20 –TMT has high sensitivity to physically small sources could be 10-100x, depending on size (and wavelength) How small are primordial objects? –At z ~ 6.5 some are <= 80-100 mas –Some gravitationally lensed sources are ~ 30mas Lensed galaxies at z ~5.7 (Ellis et al. 2001) Unlensed sizes ~ 150pc or < 30mas

46. October 4, 2015 TMT.IAO.PRE.09.035.REL01 46 Example of future instrument: MIRES Mid-IR Echelle Spectrometer Mid-IR Diffraction Limited Spectrometer Fed by “MIRAO” or “AM2” LGS or NGS 5000< R <100000 with diffraction-limited slit 8 - 18 microns, goal: 3.5 - 28 microns Goal: 10” science imager operating at 5mu with 17mas pixels Feasibility Study team Co-PIs: Alan Tokunaga (UH), Jay Elias (NOAO) –19 team members from 10 US institutions: UH, NOAO, NRL, UCD, Gemini, Caltech, Lowell Obs, JPL, Goddard, UT Austin – + Chris Packham(Florida) and Y Okamoto (Tokyo) MIRAO MIRES

47. October 4, 2015 TMT.IAO.PRE.09.035.REL01 47 MIRES MIRES enables “D 4 ” science that cannot be duplicated on smaller telescopes or from space sensitivity resolution Line sensitivity ~MIRI-JWST 5x spatial resolution of JWST