the tmt instrumentation program brent ellerbroek and luc simard pre-spie 2010 tmt instrumentation...

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

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 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


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 instrumentsCompletely integrated system

– Fast (< 5 min) switch between targets with same instrument> 50% sky coverage at galactic poles

Narrow-Field IR AO System (NFIRAOS):TMT’s Early-Light Facility AO system

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

•(WIRC)

•NFIRAOS•IRMS

•(NIRES)

•IRIS


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)


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

HROS-CASA

IRMOS-UFWFOS-HIA

HROS-UCSCMIRES

IRMOS-CIT

IRIS

PFI

7

People


Early Light Instruments


InfraRed Imaging Spectrometer(IRIS)

http://irlab.astro.ucla.edu/iris/index.html

http://www.tmt.org/docs/WWW_IRIS_DRF01.doc

Also see J. Larkin’s presentation




IRIS Top-Level Requirements


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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)

Motivation for IRIS

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.)Keck AO images

M31 Bulge with 0.1” grid (Graham et al.)

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


Overall Field Geometry

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

•18”

Probe Arms

4” Fields 0.004” pixels


Exploded View of

IRIS Assembly

On-Instrument Wavefront Sensors

Probe arm

Camera

Dewar

IRIS Dewar

Attachment

Platform

Probe

arm

Probe

Rotational Stage

NFIRAOS Interface

Mature mechanical design ready for probe arm prototyping

Thermal Jacket

Platform Hexapod Support


IRIS Science Dewar

Entrance

Φ = 2m


Camera TMA

Lenslet

50mas slicer

Grating turret

4kx4k spectrograph

detector

Slicer IFU

Slicer collimator

Lenslet collimator

Schematic view Solid ModelImager channel

IRIS Imager and Spectrometer


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)

Point Source Sensitivities

Filter Scale (mas) Exp. Time (secs)

Number of Frames

Magnitude (AB)

J 4 900 4 24.1

H 4 900 4 23.7

K 4 300 12 22.9

Filter Exp. Time (secs)

Number of Frames

Magnitude (AB)

J 900 4 27.3

H 900 4 26.2

K 900 4 25.5

•S/N ~10•S/N ~10

S/N ~100S/N ~100Source: S. Wright &

B. Barton, 2009

CFHT/WIRCAM

KAB = 24.5 (S/N=5)

t = 30 hours !!

Wide-Field Optical Spectrometer(WFOS)

http://www.tmt.org/docs/WWW_WFOS_DRF01.doc

Also see B. Bigelow’s presentation


WFOS Top-Level Requirements

WFOS(-MOBIE) Team

Rebecca Bernstein (UCSC), Principal InvestigatorBruce Bigelow (UCSC), Project ManagerChuck Steidel (Caltech), Project ScientistScience 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 wayDifferent 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.

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WFOS-MOBIE Echellette Design

Spectral footprint in higher dispersion mode - 3’’ slits spaced

25’’ apart, five orders

MOBIE can trade multiplexing for expanded wavelength coverage

in its higher dispersion mode

Mirror

TMT Focal

Plane

Single field, blue and red arms

23

WFOS-MOBIE Examples of Spectral Resolution Options


24

WFOS-MOBIE Science Field Geometry

Multi-object mask making simulation

Source: 2008 WFOS-MOBIE Feasibility Study Operational

Concepts Definition Document

WFOS-MOBIE Schematic View

InfraRed Multi-slit Spectrometer(IRMS)

http://www.tmt.org/docs/WWW_IRMS_DRF01.doc

http://irlab.astro.ucla.edu/mosfire/




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InfraRed Multi-slit Spectrometer (IRMS)(aka 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”

– 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

IRMS and NFIRAOS

Slit width

H-band over whole 120” field


IRMS Slit Unit & Field

2’ diameter

• Detector area

• CSEM configurable slit unit• Slits formed by opposing bars• Up to 46 slitlets• Reconfigurable in ~3 minutes


MOSFIRE in Caltech Lab

“TMT prototype” MOSFIRE integration and test proceeding well

TMT First Decade Adaptive Optics


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)

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 m– 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

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PFI Block Diagram

34


IRMOS Block

Diagram (UF

Concept)

35LGS WFS

NGS WFSMEMS DM


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

36Distance from Center FoV

Zen

ith A

ngle


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

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MIRAO Optical Schematic

LGS WFSs

DM

Light from TMT

Output to Instrument


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,. …


Required AO Component Advances by Application

System or AO mode

Lasers IR det.

Piezo DMs

MEMs AM2 RTC HW

RTC algs.

WFS concepts

MIRAO Replaces piezo., reduces emission

PMOS 642 small stroke

Higher order

MOAO DM control

MOAO (small stroke)

IRMOS 642 larger stroke

Replaces piezo.

Higher order

MOAO DM control

MOAO

GLAO Required

NFIRAOS+ Pulsed 50w?

1202

large stroke

Reduces piezo stroke

Higher order

Dynamic refocus

PFI Big, fast, quiet

1282 small stroke

Replaces piezo

TBD (green to yellow)

Prediction and calibration

Pyramid, post-corona-graphic40


Future Instrumentation Development


Defining the TMT Instrumentation Development Program

Observatory ContextRequirements and architecturesInterfaces (optical, mechanical, power and cooling, data and communications)Common standards and practicesDefinition of development and delivery phasesPlanning and Management Practices (costing, schedule, risks, etc.)

Development process

ProcurementParticipation (TMT partners, broader community)Support for funding requestsWork package agreementsModels and phasing scenarios


Defining the TMT Instrumentation Development Program

Instrumentation Development OfficeTasksPersonnel

Development fundingFunding levelsTypes of source

Incentives


Future Instrumentation Development:Proposed Process

Community explorations (scientific and technical)Consultations (e.g., workshops)Mini-studies

SAC prioritization“Cornerstone” of instrumentation developmentWell-defined metrics for science, technical readiness, schedule and costBalance between AO systems and science instruments

Conceptual Design StudiesEstablishment of Board guidelines on scope and costCall for ProposalsStudy phase (two ~one-year competitive studies for each instrument)External ReviewsSAC evaluation and recommendations to the Board


Future Instrumentation Development:Proposed Process (cont.)

Instrumentation contract awardsObservatory (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


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 instruments4 core FTEs in current operations planInstrument development budget of ~$10 M / year


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


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.


the tmt instrumentation program brent ellerbroek and luc simard pre-spie 2010 tmt instrumentation...

Documents

light facility ao

instrument synergies

decade of tmt operations

conjugate ao system

au galactic center

ucscmiresirmoscitiris

following instruments

au typical galactic