W. M. Keck Observatory’s Next Generation Adaptive Optics Preliminary Design & Path Forward Peter...

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W. M. Keck Observatory’s W. M. Keck Observatory’s Next Generation Adaptive Next Generation Adaptive Optics Optics Preliminary Design & Path Forward Preliminary Design & Path Forward Peter Wizinowich, Sean Adkins, Rich Dekany, Peter Wizinowich, Sean Adkins, Rich Dekany, Don Gavel, Claire Max Don Gavel, Claire Max for NGAO Team: for NGAO Team: R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Kupke, R. Kupke, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Neyman, C. Neyman, S. Panteleev, M. Pollard, M. Reinig, T. Stalcup, S. Thomas, S. Panteleev, M. Pollard, M. Reinig, T. Stalcup, S. Thomas, M. Troy, M. Troy, K. Tsubota, V. Velur, K. Wallace, E. Wetherell K. Tsubota, V. Velur, K. Wallace, E. Wetherell SSC, Waimea SSC, Waimea July 7, 2010 July 7, 2010
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Transcript of W. M. Keck Observatory’s Next Generation Adaptive Optics Preliminary Design & Path Forward Peter...

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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NGAO on Nasmyth Platform

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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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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)

Path ForwardPath Forward

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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