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W. M. Keck Observatory’sW. M. Keck Observatory’sNext Generation Adaptive OpticsNext Generation Adaptive Optics
Preliminary Design & Path ForwardPreliminary Design & Path Forward
Peter Wizinowich, Sean Adkins, Rich Dekany, Peter Wizinowich, Sean Adkins, Rich Dekany, Don Gavel, Claire MaxDon Gavel, Claire Max
for NGAO Team:for NGAO Team: R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Kupke, R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Kupke, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Neyman, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Neyman,
S. Panteleev, M. Pollard, M. Reinig, T. Stalcup, S. Thomas, M. Troy, S. Panteleev, M. Pollard, M. Reinig, T. Stalcup, S. Thomas, M. Troy, K. Tsubota, V. Velur, K. Wallace, E. WetherellK. Tsubota, V. Velur, K. Wallace, E. Wetherell
SSC, WaimeaSSC, WaimeaJuly 7, 2010July 7, 2010
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Flowed-Down Key Architectural FeaturesG
alax
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Near diffraction-limited in near-IR
AO correction at red wavelengths
Increased sky coverage
Improved sensitivity
Improved contrastImproved photometric
accuracyImproved astrometric
accuracy
ImagingIntegral field spectroscopy
Key Science Drivers Key Architectural Features
Key New Science Capabilities
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NGAO System Architecture
Key Features:1. Fixed narrow field laser tomography2. AO corrected NIR TT sensors3. Cooled AO enclosure4. Cascaded relay5. Combined imager/IFU instrument
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DAVINCI – Imager & IFS
Entrance window
Coronagraph mask wheel
Imager detector
headImager/IFS
selector mirror
Pupil imager wheel
Filter and pupil mask wheels
IFS detector head
Grating selector wheel
• On axis imager 28.7" x 28.7" FOV– 7 mas pixel scale
• On axis selectable IFS– 50 mas spatial scale FOV 5.6" x 3"
– 35 mas, FOV 3.92" x 2.1"
– 10 mas, FOV 1.12" x 0.6"
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Science Case Performance Summary
10 mas
35 mas
50 mas
70 mas
1Galaxy Assembly K 158 4.9 180 77% 4% 36% 56% 75%
2 Nearby AGN Z 158 4.8 176 21% 8% 29% 30% 31%
3aGalactic Center Imaging K 208 2.2 212 69% 4% 31% 48% 65%
3bGalactic Center Spectra H 191 2.4 195 57% 5% 38% 52% 59%
4 Exo-planets H 155 2.9 162 68% 6% 46% 62% 71%5 Minor Planets Z 157 4.7 175 21% 8% 29% 30% 31%6 Io Z 116 2.1 119 48% 14% 51% 53% 53%
Ensquared Energy in Spaxel
Case # Science Case
Science Band
RMS High-order
Wavefront Error (nm)
RMS Tip-Tilt Error
(mas)
Effective RMS
Wavefront Error (nm)
Strehl Ratio
Galaxy assembly: 30º zenith angle, 60º galactic latitude, 30 min integ.
AO correction of IR tip-tilt stars has big benefit for sky coverage
Galaxy assembly science case
Current Keck TT
Current Keck EE NGAO TT
NGAO EE
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K-band Strehl Ratio
AO performance comparison
Liu's K2 LGS AO Data K2 LGS AO Model NGAO Model
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NGAO changes the Keck AO observing experience
Monte Carlo performance estimate simulating 44 nights observing (Galaxy Assembly science case), drawing random values for r0, wind speed, sodium
abundance, and zenith angle
Includes comparison with M. Liu’s measured K2 LGS data (<SR> = 17%), the model prediction for K2 LGS (<SR> = 20%), and NGAO predict (<SR> = 70%)
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AO performance comparison
Liu's K2 LGS AO Data K2 LGS AO Model NGAO Model
Path to Early Science Benefits from NGAO is Already Under Way - 1
• NGAO laser launch telescope– NSF-MRI (Aug/09) funding to procure & implement a K2 center
launch telescope
• NGAO laser– Preliminary designs completed (Dec/09) from 2 vendors.
Collaboration with ESO, AURA, GMT & TMT. TOPTICA/MPBC selected to begin final design.
– MRI proposal submitted to procure & implement 1st NGAO laser on K2. Collaboration with TMT & ESO.
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Path to Early Science Benefits from NGAO is Already Under Way - 2
• PSF reconstruction– Collaboration with Gemini & U. Groningen to demonstrate on-axis
NGS AO PSF reconstruction on Gemini & Keck– Plan to implement off-axis LGS AO PSF reconstruction with Keck– MASS/DIMM implemented (Sept/09) as a Mauna Kea facility
• Focal anisoplanatism reduction– Risk reduction to demonstrate 20% reduction using Cn2 data
• Tip-tilt vibration reduction– Risk reduction plan to prototype parametric oscillator on K2 AO
• NIR tip-tilt sensing (no object selection or AO correction)– ATI (Jun/10) funding to implement a near-IR tip-tilt sensor
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Keck AO First TAC-allocated Science Milestones
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Major Keck AO Science Capability Milestones
Future
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Cost Estimate versus Funding
• Need a path to $49.3M (then-year $) or $44.5M (FY10 $)• Includes ~$11M (then-year) for detailed design with contingency
NGAO System Total Committed Proposed Required
System Design (WMKO) 1244 1244 0Preliminary Design (TSIP) 2845 3031 -186Detailed Design 7906 7906Full Scale Development 18932 18932Delivery & Commissioning 2903 2903Contingency 7251 7251
NGAO Total = 41080MRI Laser Launch Telescope 1535 1535 0MRI Laser 3214 3214 0
NGAO Proposal Total = 4748DAVINCI Prel. Design (TSIP) 245 245 0DAVINCI PD & DD 885 885DAVINCI FSD & DC 8708 8708Contingency 2858 2858
NGAO Instrument Total = 12696Overall Total = 58524 6054 3214 49257
Funding ($k)
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Funding Options (Project Perspective)
1. Proceed with full NGAO plan (as outlined at PDR & endorsed by Review Committee)
or
2. Proceed with staged implementation on the path to the full NGAO system, with clear near-term science return
We will discuss each of these in turn
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1. Proceed with Full NGAO Plan
• Potential path to significant funding (dependent on Astro2010 report):
– Submit an unsolicited proposal to MPS’s existing “Mid-Scale Instrumentation Program” to fund detailed design• This program has funded multiple AST programs (Atacama
Cosmology Telescope, Murchison Wide-Field Array, LSST design, GSMT development, etc.)
– Develop a proposal to NSF for full funding
– Continue private fundraising efforts
• This is the path recommended by the NGAO team– We would continue to seek early science / staged
opportunities
NGAO has demonstrated that it can successfully compete & collaborate
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Demonstrated fund raising & leveraging successes:Category
Awarded Source $k Source $kNGAO Preliminary Design TSIP 3776Laser Preliminary Design GSMT 300 ESO 700Laser launch telescope MRI 1356PSF reconstruction CfAO 20 Gemini 42
U. Groningen 43MASS/DIMM on Mauna Kea TMT donation 800
CFHT/UH install 200Near-IR tip-tilt sensor ATI 1720
Total = 7172 1785SubmittedLaser design + 1 unit MRI 3318 TMT (cash) 600
ESO (NRE) 2599
NSF Leveraged
One (extreme) interpretation: 36 nights $9.0M or $249k/night
2. Staged Implementation Path to NGAO
• Significant “development chunks” that are on the path to the full NGAO system, with clear near-term science return
• Criteria for selection: each development stage should accomplish the following goals, with equal weight:
– It should provide early science return to the WMKO community
– It should be on the path to the full NGAO project
• In addition a proposal should accomplish the following:
– It should help keep the NGAO team working together on NGAO goals
– It should reduce NGAO risk
– It should allow us to leverage the work of others, especially TMT
• Potential funding sources: NSF ATI, MRI, TSIP & private fundraising past the January 2011 deadline
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Preliminary list of possible early “stages”
1. New laser (if not funded by MRI)
2. Develop PSF reconstruction techniques– Will be useful to all Keck AO users– Key to precision photometry and astrometry with NGAO
3. Increase sky coverage of existing AO system by building an AO feed to the new infrared tip-tilt sensor– Would serve as prototype for NGAO’s tip-tilt arms
4. Implement laser tomography on existing AO system– Increase Strehl & enclosed energy by reducing “cone effect”– Risk/cost reduction collaboration opportunities on RTC & WFS
camera
In support of decision making NGAO team & NSAT will evaluate science return, feasibility & cost of “stages”
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In ClosingIn Closing
• Keck AO has been very successful scientifically
• NGAO preliminary design received a very strong endorsement
• NGAO can successfully compete for & leverage Federal funding
• NGAO Team ready to compete for funding & to deliver this key element which is “critical to WMKO’s future as a facility producing forefront science” (NGAO Review Panel)
Keck AO NGAO