1. The TMT Instrumentation Program
Brent Ellerbroek and Luc Simard
Pre-SPIE 2010 TMT Instrumentation Workshop
San Diego, June 26, 2010
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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
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3. TMT Instrumentation and Performance 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
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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
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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)
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6. Feasibility studies 2005-6 (concepts, requirements, performance,…)
IRIS
MIRES
HROS-UCSC
HROS-CASA
PFI
WFOS-HIA
IRMOS-UF
IRMOS-CIT

7. People
TMT discovery space: main goal is to show that AO is a must to get to the “really good stuff”
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8. Early Light Instruments
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9. InfraRed Imaging Spectrometer (IRIS)
Also see J. Larkin’s presentation
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10. IRIS Top-Level Requirements
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11. Motivation for IRIS
Unprecedented ability to investigate objects on small scales:
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)
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.)

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
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13. Overall Field Geometry
Imager Field is on-axis
17” field 0.004” pixels
Spectrographs concentric
18” off-axis
2 Coarse Scales (Slicer)
45x90x~2000 elements
2 Fine Scales (Lenslet)
112x128x500 elements
Probe Arms
4” Fields 0.004” pixels
18”
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14. Exploded View of IRIS Assembly

15. On-Instrument Wavefront Sensors
NFIRAOS Interface
Probe arm
Platform
Probe
Rotational Stage
Camera
Dewar
Probe
arm
Mature mechanical design ready for probe arm prototyping
IRIS Dewar
Attachment
Platform Hexapod Support
Thermal Jacket
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16. IRIS Science Dewar
Entrance
Φ = 2m
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17. IRIS Imager and Spectrometer
Camera TMA
Lenslet
50mas slicer
Grating turret
4kx4k spectrograph detector
Slicer IFU
Slicer collimator
Lenslet collimator
Schematic view
Imager channel
Solid Model
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18. 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)
Filter
Scale (mas)
Exp. Time (secs)
Number of Frames
Magnitude (AB) J 4
900
24.1 H
23.7 K
300 12
22.9
S/N ~10
Filter
Exp. Time (secs)
Number of Frames
Magnitude (AB) J
900 4
27.3 H
26.2 K
25.5
CFHT/WIRCAM
KAB = 24.5 (S/N=5)
t = 30 hours !!
S/N ~100
Source: S. Wright & B. Barton, 2009

19. Wide-Field Optical Spectrometer (WFOS)
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
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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)
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27. InfraRed Multi-slit Spectrometer (IRMS) (aka Keck/MOSFIRE on TMT)

28. H-band over whole 120” field
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
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29. IRMS Slit Unit & Field CSEM configurable slit unit
Detector area
2’ diameter
CSEM configurable slit unit
Slits formed by opposing bars
Up to 46 slitlets
Reconfigurable in ~3 minutes
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30. “TMT prototype” MOSFIRE integration and test proceeding well
MOSFIRE in Caltech Lab

31. TMT First Decade Adaptive Optics
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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 range
Order ~128 correction; coronagraphy, advanced WFS detectors/concepts
2006 feasibility study by LLNL/JPL
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34. PFI Block Diagram
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35. IRMOS Block Diagram (UF Concept)
MEMS DM
NGS WFS
LGS WFS
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36. Distance from Center FoV
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
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37. Potential Facility AO Upgrades
Mid IR AO facility (MIRAO)
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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38. MIRAO Optical Schematic
Light from TMT
Output to Instrument DM
LGS WFSs
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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,. …
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40. 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.
MOAO
GLAO
Required
NFIRAOS+
Pulsed 50w?
1202 large stroke
Reduces piezo stroke
Dynamic refocus
PFI
Big, fast, quiet
1282 small stroke
Replaces piezo
TBD (green to yellow)
Prediction and calibration
Pyramid, post-corona-graphic
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41. Future Instrumentation Development
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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
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43. Defining the TMT Instrumentation Development Program
Instrumentation Development Office
Tasks
Personnel
Development funding
Funding levels
Types of source
Incentives
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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
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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
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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
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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
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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.
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