The TMT Instrumentation Program Brent Ellerbroek and Luc Simard Pre-SPIE 2010 TMT Instrumentation...
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Transcript of 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
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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
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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
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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
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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
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
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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
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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
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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
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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
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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(-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.
22
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
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WFOS-MOBIE Science Field Geometry
Multi-object mask making simulation
Source: 2008 WFOS-MOBIE Feasibility Study Operational
Concepts Definition Document
InfraRed Multi-slit Spectrometer(IRMS)
http://www.tmt.org/docs/WWW_IRMS_DRF01.doc
http://irlab.astro.ucla.edu/mosfire/
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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
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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
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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
33
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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
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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
37
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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,. …
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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
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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
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Defining the TMT Instrumentation Development Program
Instrumentation Development OfficeTasksPersonnel
Development fundingFunding levelsTypes of source
Incentives
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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
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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
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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
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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
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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.
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