the tmt instrumentation program david crampton meeting with chinese delegation pasadena june 4, 2009...

The TMT Instrumentation Program

David CramptonMeeting with Chinese Delegation

PasadenaJune 4, 2009

([email protected])

April 21, 2023TMT.IAO.PRE.09.035.REL01

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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


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Key Requirement: to realize the full scientific potential of a diffraction-limited 30m telescope


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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 lightEnsure that entire Observatory system is optimized to produce the best possible scienceEstablish telescope and observatory requirements and interfaces for instruments of all typesEstablish costs and schedulesUnderstand risks and mitigation strategiesDevelop plans for ongoing instrument development


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Instrumentation Philosophy

Using world-class teams, develop best possible instrument concepts to meet the scientific requirements– Attempt to engage whole astronomical community, including

international partnershipsPlan 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


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CapabilitySpectral

ResolutionScience 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


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Instruments are all located on two large Nasmyth structures

HROS

WFOS

IRMOS

MIRAO/

MIRES

APS

PFI

NFIRAOS

IRIS (bottom port)

WIRC

NIRES-B


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NFIRAOS feeds 3 instruments

Strehl Ratio Band SRD (120 nm) Baseline (177

nm) Baseline + TT

R 0.313 0.080 0.052 I 0.411 0.145 0.105 Z 0.566 0.290 0.236 J 0.674 0.424 0.366 H 0.801 0.617 0.569 K 0.889 0.774 0.742

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)


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TMT Instrument Feasibility Studies2005-6

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 2005Feasibility 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


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Feasibility studies 2005-6 (concepts, requirements, performance,…)

HROS-CASA

IRMOS-UFWFOS-HIA

HROS-UCSCMIRES

IRMOS-CIT

IRIS

PFI


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Feasibility studies 2005-6 (concepts, requirements, performance,…)

HROS-CASA

IRMOS-UFWFOS-HIA

HROS-UCSCMIRES

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.


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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


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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!


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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.


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IRIS Conceptual Design Team

James Larkin (UCLA), PI, Lenslet IFSAnna Moore (Caltech), co-I, Slicer IFSRyuji Suzuki, Masahiro Konishi, Tomonori Usuda (NAOJ), ImagerBetsy Barton (UC Irvine), Project ScientistScience 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


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Motivation for IRIS

Should be the most sensitive astronomical IR spectrograph ever builtUnprecedented 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


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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)

Imager Lenslet and slicer foreoptics

Common camera and detector


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WFOS Team

Rebecca Bernstein (UCSC), PIBruce Bigelow (UCSC), PMChuck Steidel (Caltech), PSScience 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.


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WFOS-MOBIESeeing-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


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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


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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


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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


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


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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)


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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)


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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


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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 - D4 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


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Development of Future Instruments


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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


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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


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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


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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.


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Detection of Habitable TerrestrialPlanets Around Nearby G,K,M Stars

Gliese 876 M4V at 15pc

A 7.5 earth-mass rock…

5 MEarth 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


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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


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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!


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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


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Typical Development Cycle(2 instruments, one simple, one complex)

2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 2021 2022

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

Commission


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Cartoon of development funding profile (Fiscal Years, $M2009)

Instruments are commissioned in the blue-filled cells.

FY INS

14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 Sum

NIRES HROS

3.0 3.0 9.3 9.3 9.3 9.3 9.3 9.3 NIRES HROS 62

MIRES NIRES-R

3.0 3.0 9.2 9.2 9.2 9.2 9.2 9.2 MIRES NIRES-R

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PFI 2.7 2.7 8.6 8.6 8.6 8.6 8.6 8.6 PFI 57 IRMOS* 2.2 11.4 11.4 11.4 11.4 11.4 11.4 71 NFIRAOS+ WIRC

3.4 3.4 7

Total 3.0 3.0 12.3 12.3 18.5 18.5 21 21 18 20 20 20 20 20 15 15 258


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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)


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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


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HROS, NIRES, WFOS

IRIS, IRMOS

PFIMIRESNIRESHROSIRIS

WFOS

IRIS

IRMOS


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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.


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NFIRAOS+LGSF+IRIS 2018: Ready for first AO light


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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


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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


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MIRES

• MIRES enables “D4” science that cannot be duplicated on smaller telescopes or from space

• sensitivity• resolution

• Line sensitivity ~MIRI-JWST• 5x spatial resolution of JWST

the tmt instrumentation program david crampton meeting with chinese delegation pasadena june 4, 2009...

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