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Next Generation Adaptive Optics (NGAO) System Design Phase Update

Next Generation Adaptive Optics (NGAO) System Design Phase Update. Peter Wizinowich, Rich Dekany, Don Gavel, Claire Max Science Case Presenters: Brian Cameron, David Law, Jessica Lu, Phil Marshall, Chuck Steidel, Tommaso Treu Technical Team: Sean Adkins, Brian Bauman, Jim Bell,

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Next Generation Adaptive Optics (NGAO) System Design Phase Update

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  1. Next Generation Adaptive Optics (NGAO)System Design Phase Update Peter Wizinowich, Rich Dekany, Don Gavel, Claire Max Science Case Presenters: Brian Cameron, David Law, Jessica Lu, Phil Marshall, Chuck Steidel, Tommaso Treu Technical Team: Sean Adkins, Brian Bauman, Jim Bell, Antonin Bouchez, Matthew Britton, Jason Chin, Ralf Flicker, Erik Johansson, David Le Mignant, Chris Lockwood, Liz McGrath, Anna Moore, Chris Neyman, Viswa Velur Keck Strategic Planning Meeting September 20, 2007

  2. Presentation Sequence 1:00 pm WMKO Strategic Plan & NGAO (Wizinowich) 1:10 pm NGAO System Design Phase Status 1:15 pm Science Cases & Requirements • Overview (Max) • Precision astrometry at the Galactic Center & in sparse fields (Cameron & Lu) • High redshift galaxies with multiple IFU’s (Steidel & Law) • Gravitationally lensed galaxies with single IFU’s (Marshall & Treu) 2:20 pm System Architecture (Dekany) 2:30 pm Discussion • Potential Topics 3:00 pm Done

  3. WMKO Strategic Plan & NGAO

  4. Keck Strategic Plan: Twenty-year strategic goals • Leadership in high angular resolution astronomy • Leadership in state of the art instrumentation • Highly efficient observing • Complementarity with ELTs • NGAO supports all of these!

  5. Keck AO Strategic Plan: NGAO • AO strategic plan established by Keck AO Working Group in Nov/02 &reaffirmed in Sept/04:“AOWG vision is that high Strehl, single-object, AO will be the most important competitive point for Keck AO in the next decade.” • Sept/05: New AOWG tasked by Observatory & SSC to develop science case for Keck NGAO. • Jun/06. NGAO proposal approved. Multi-object also emphasized

  6. Substellar binaries Keck AO Science Productivity 126 NGS & 30 LGS

  7. Key new capabilities for NGAO • Dramatically improved near-IR performance • Significantly higher Strehls ( 80% at K)  improved sensitivity • Lower backgrounds  improved sensitivity • Improved PSF stability & knowledge  improved photometry, astrometry & companion sensitivity • Increased sky coverage & Multiplexing • Improved tip/tilt correction  improved sky coverage • Multiplexing  dramatic efficiency improvements  Much broader range of science programs • AO correction at red wavelengths • Strehl of 15 - 25% at 750 nm  highest angular resolution of any existing filled aperture telescope • Instrumentation to facilitate the range of science programs

  8. NGAO Current NGS Current LGS Key performance metrics: Strehl vs. observing wavelength Ca Triplet H

  9. System Architecture • Tomography to measure wavefronts & overcome cone effect • AO-corrected, IR tip-tilt stars for broad sky coverage • Closed-loop AO for 1st relay • Open-loop AO for deployable IFUs & 2nd relay

  10. NGAO System Design PhaseStatus

  11. NGAO System Design Phase System Design Phase. Oct/07 to Apr/08. Executive Committee established to manage this phase: Wizinowich (WMKO, chair), Dekany (Caltech), Gavel (UCSC), Max (UCSC, project scientist) Deliverables: Science & Observatory requirements & flow down to system requirements Performance budgets, functional requirements, system & subsystem architectures Management plan for remaining NGAO phases 11

  12. System Design Milestones Requirements  Performance Budgets + Trade Studies  System Architecture + Functional Requirements  Subsystem Design + Functional Requirements  Management Plan

  13. System Design Products • All products maintained at NGAO TWiki site (just Google NGAO) including: • Requirements documents (Science case, System & Functional) • Performance budget reports (wavefront error & encircled energy, astrometry, photometry, companion sensitivity & throughput/emissivity) • Model assumption & validation reports (total of 14) • Trade study reports (total of 23) • Management plans & reports Goal of NGAO shared-risk science in 2013

  14. Science Cases & Requirements

  15. Outline • What is complementary and scientifically unique about Keck NGAO? • JWST, ALMA, TMT • Other ground-based observatories • “Science Cases” for NGAO: what are “science requirements” that will guide the design?

  16. Key new capabilities for NGAO • Dramatically improved near-IR performance • Increased sky coverage & Multiplexing • AO correction at red wavelengths • Instrumentation to facilitate the range of science programs

  17. Complementary to JWST, ALMA • JWST: 2013 • Much higher sensitivity longward of K band • NGAO emphasizing wavelengths > K band • JWST: “Expect same resolution as HST below 2 m” • NGAO has clear resolution advantage • No multi-object IFU capability • ALMA: 2012 • Spatial resolution as low as 0.01 to 0.1 arc sec (!) • Complementary data on dust & cold gas Our goal is to position NGAO to build on, and complement, JWST & ALMA discoveries

  18. Complementary to TMT • TMT IRMS: AO multi-slit, based on MOSFIRE • Slits: 0.12” and 0.16”, Field of regard: 2 arc min • Lower backgrounds: 10% of sky + telescope • NGAO with multiplexed deployable IFU’s • Multi-object AO  better spatial resolution (0.07”) over full field • Backgrounds:  30% of sky + telescope • Pros for TMT: lower backgrounds, higher sensitivity • Pros for NGAO: higher spatial resolution, 2D information, better wide field performance

  19. Complementary with other ground-based observatories • Other ground-based observatories are largely focusing on wide fields with modest performance, or on very high contrast AO • “Wide” field (by AO standards): • Gemini South: Multi-conjugate AO • VLT: Ground layer AO • High Contrast: • Gemini Planet Imager • VLT SPHERE

  20. Scale of new VLT AO projects is really big • Hawk-I: 2012 with AO • K-band imager, 7.5’ x 7.5’ field • MUSE visible multi-IFU: 2012 • 1' field, x 2 seeing improvement • MUSE visible narrow field IFU: 2012 • 7.5” field, ~5% Strehl at 750 nm • NGAO must strike balance between scale/cost, risk, and science return. • Lesson from these VLT projects: have courage, but be realistic too

  21. Outline • What is complementary and scientifically unique about Keck NGAO? • JWST, ALMA, TMT • Other ground-based observatories • “Science Cases” for NGAO: what are “science requirements” that will guide the design?

  22. Categorize science cases into 2 classes • Key Science Drivers: • These push the limits of AO system, instrument, and telescope performance. Determine the most difficult performance requirements. • Science Drivers: • These are less technically demanding but still place important requirements on available observing modes, instruments, and PSF knowledge.

  23. Key Science Drivers(in order of distance) • Minor planets as remnants of early Solar System • Planets around low-mass stars • General Relativity at the Galactic Center • Black hole masses in nearby AGNs • High-redshift galaxies

  24. Key Science Drivers(in order of distance) • Minor planets as remnants of early Solar System • I-band AO; high contrast; astrometry • Planets around low-mass stars • High contrast at J, H bands • General Relativity at the Galactic Center • Precision astrometry and radial velocities • Black hole masses in nearby AGNs • Spatially resolved spectra at Ca triplet (8500 Å) • High-redshift galaxies • Multi-IFU spectroscopy; low backgrounds; high sky coverage

  25. Some Science Requirements from Key Science Drivers (physical)

  26. Some Science Requirements from Key Science Drivers (performance)

  27. Instrument Priorities from Key Science Drivers • Near-IR imager • Visible imager • Near-IR IFU (OSIRIS?) • Visible IFU Narrow field: Multi-object: Deployable near-IR multi-object IFU

  28. Some Science Cases have specific observing requirements • Efficient surveys: (e.g. asteroid companions and planets around low-mass stars) • Optimizing overall science output of the Observatory • “Seeing” and AO correction are variable • Requirements on ability to switch to NGS, and to other instruments • What kinds of “flexible observing” might be appropriate?

  29. Science Requirements from Science Drivers (short summary) • An “eye test” here, but printed out on your handout sheets. Please send us your input!

  30. Science Drivers(in order of distance) • Asteroid size, shape, composition • Giant Planets and their moons • Debris disks and Young Stellar Objects • Astrometry in sparse fields • Resolved stellar populations in crowded fields • QSO host galaxies • Gravitationally lensed galaxies Requirements based on these Science Drivers are still under discussion - we need your input!

  31. NGAO will allow us to tackle important, high-impact science • Near diffraction-limited in near-IR (Strehl >80%) • Direct detection of planets around low-mass stars • Astrometric tests of general relativity in the Galactic Center • Structure & kinematics of subcomponents in high redshift galaxies • Vastly increased sky coverage and multiplexing • Multi-object IFU surveys of distant galaxies • AO correction at red wavelengths (0.7-1.0 mm) • Scattered-light studies of debris disks and their planets • Masses and composition of asteroids and Kuiper Belt objects • Mass determinations for supermassive black holes

  32. Science Case Presentations today • Precision astrometry at Galactic Center & in sparse fields • Brian Cameron and Jessica Lu • Spectroscopy of high-redshift galaxies • Chuck Steidel and David Law • Gravitationally lensed galaxies • Tommaso Treu and Phil Marshall Intended to illustrate NGAO science requirements development process

  33. NGAO System Design: System Architecture

  34. SystemArchitecture

  35. NGAO Fields of Regard 5 LGS variable radius asterism 180" FoR for tip-tilt star selection 202" LGS patrol range 3 tip/tilt stars 3 tip/tilt stars 5 LGS on 11” radius Roving LGS Central LGS Multi-object deployable IFU FoV 30 arcsec 120 arcsec 1st Relay / DNIRIField of Regard 2nd Relay / Precision AO Field of Regard

  36. Woofer DM 589 nm Light f/15 AO Relay Telescope elevation bearing LGS OSM K‑mirror image de-rotator Visible imager Near-IR imager Keck I or II right Nasmyth platform OMU Bench LGS wavefront sensors on focus stages IFU and tip-tilt OSM Narrow field selection mirror 2 channel IFU spectrograph (1 of 3) Tip-tilt sensor (1 of 3) Near-IR IFU (OSIRIS) f/45 narrow field AO relay System Design Progressing

  37. Conclusion: NGAO Capabilities • Dramatically improved near-IR performance • Significantly higher Strehls ( 80% at K)  improved sensitivity • Lower backgrounds  improved sensitivity • Improved PSF stability & knowledge  improved photometry, astrometry & companion sensitivity • Increased sky coverage & Multiplexing • Improved tip/tilt correction  improved sky coverage • Multiplexing  dramatic efficiency improvements  Much broader range of science programs • AO correction at red wavelengths • Strehl of 15 - 25% at 750 nm  highest angular resolution of any existing filled aperture telescope • Instrumentation to facilitate the range of science programs Enables wide variety of new science within interests of Keck Community

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