Keck All Sky PrecisionAdaptive Optics · the summit of Mauna Kea has always had within the...
1
Keck All Sky Precision Adaptive Optics W. M. Keck Observatory ABSTRACT We present the goals, status and plans for the Keck All sky Precision Adaptive optics (KAPA) program. The program includes four key science projects, an upgrade to the Keck I laser guide star (LGS) adaptive optics (AO) facility to improve image quality and sky coverage, AO telemetry based PSF estimates for all science exposures, and an educational component focused on broadening the participation of women and underrepresented groups in instrumentation. All of these elements have pathfinder relevance for the ELTs. For the purpose of this conference we will focus on the AO facility upgrade which includes implementation of a new laser, wavefront sensor and real-time controller to support laser tomography, the laser tomography system itself, and modifications to an existing near-infrared tip-tilt sensor to support multiple NGS tip-tilt and focus measurements. KAPA Team Technical Team 1 : K. Casey, J. Chin (Proj. Manager), S. Cetre, C. Correia, S. Lilley, S. Ragland, E. Wetherell, P Wizinowich (PI) Science Team: A. Ghez (Science Legacy Lead) 4 , M. Liu 5 , J. Lu (Proj. Scientist) 3 , D. Mawet 6 , C. Max 2 , M. Morris 4 , T. Treu 4 , S. Wright 7 Education Lead: L. Hunter 2 1 WMKO, 2 UCSC, 3 UCB, 4 UCLA, 5 UH, 6 Caltech, 7 UCSD Technical Collaborators: C. Boyer, A. Bouchez, S. Esposito, T. Fusco, J.-P. Veran Consultant: M. van Dam Laser: TOPTICA Photonics & MPB Communications RTC: Microgate, Swinburne University of Technology, Australian National University, Observatoire de Paris 90 km Laser Tomography (3 LGS asterism) • Asterism generator with a beam splitter assembly to provide 3 LGS • 6.4" radius beam separation • Field rotation is provided • Individual closed loop tip/tilt control from wavefront sensor • 3 LGS spots on single OCAM2k camera detector • Operational scenarios on WFS • Single NGS/LGS centered on the optical axis, centered on the detector • Three LGS beams separated by 120°, offset from reducer optics optical axis by 1.691mm. Pupils on lenslet array 1. Constraining dark matter, the Hubble constant, and dark energy via strong gravitational lensing 2. Testing General Relativity and studying supermassive black hole interactions at the Galactic Center 3. Characterizing galaxy kinematics and metallicity using rare highly magnified galaxies 4. Directly studying gas-giant protoplanets around the youngest stars Performance Improvements Science Case Publicly Available Data Products Dark Matter Subhalo mass function Dark Energy Stellar velocity fields Kinematics catalog Reference frame Stellar spectral & photometric properties Internal kinematics of lensed galaxies Metallicity gradients of lensed galaxies Contrast curves List of identified candidates Imaging data Galactic Center Galaxy Evolution Gas-Giant Protoplanets Key Science Programs Akamai AstroTech KVS Postdocs Undergrad Grad Postdoc Broaden participation in instrumentation for women & URM Educational Program and Outreach ACKNOWLEDGEMENTS • The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. • Funding support for the KAPA System provided by the National Science Foundation Mid Scale Innovations Program award AST-1836016. • Funding support for the AstroTech instrumentation intensive provided by the Heising-Simons Foundation. • Keck II RTC is funded by the NSF Major Research for Instrumentation Program award AST-1727071 • The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. • Photos: Courtesy of Ethan Tweedie, TOPTICA, and WMKO staff Project Elements Laser Laser Tomography K1 RTC Upgrade NIR Tip-tilt Upgrade PSF-R for OSIRIS KAPA Science K2 RTC Upgrade Education/ Outreach Real Time Controller (Microgate) • Microgate is collaborating with Swinburne University, Australian National University, Observatoire de Paris to provide RTC • GPU based RTC with telemetry recorder storage (100TB); based on Keck II RTC Upgrade funded by NSF Major Research Instrumentation Program • Dedicated FPGA hardware to interface with existing and new AO sensors, and motion devices: pyramid WFS, SH WFS, downlink and uplink tip-tilt mirrors , IR-TT and visible TT sensors, MEMS and piezo DMs • FPGA based uXLink interface board to reduce jitter with direct DMA transfer of data into the GPUs; based on European Green Flash Project • Flexible architecture to add future hardware, modes and capabilities: sensor fusion, predictive control, PSF-R • CACAO (compute and control for AO) libraries for low latency processing; CACAO currently operating on PWS as a prototype • OCAM2K EMCCD WFS for 3 LGS on a single detector • Initial performance demonstrates <100us latency • Built-in simulator PSF-R with OSIRIS Instrument NIR Tip-tilt Upgrade 10 2″ 102″ • Upgrade existing sensor to use 3 NGS for tip- tilt • Reduces tip-tilt anisoplanatism • Implement LIFT algorithm to also provide focus • Replacement of solid state laser with a TOPTICA/MPBC fiber laser for improved reliability and sodium return • Integrate laser with existing Center Launch System • Upgrade Software Sequencer Control TOPTICA Laser and Center Launch Beam Train • PSF-Reconstruction (PSF-R) using AO telemetry, atmospheric profile and instrument characterization • Science data and PSF-R archived in Keck Observatory Archive. • Will port on-axis algorithms developed for NIRC2 after science verification • Development of OTF terms for tomography TRICK Dewar and Electronics Photo Courtesy of TOPTICA Photo Courtesy of WMKO AstroTech Development Workshop, July 15-19 at UCB Photo Courtesy of WMKO Photo Courtesy of WMKO Photo Courtesy of WMKO
Transcript of Keck All Sky PrecisionAdaptive Optics · the summit of Mauna Kea has always had within the...
Keck All Sky PrecisionAdaptive OpticsW. M. Keck Observatory
ABSTRACT We present the goals, status and plans for the Keck All sky Precision Adaptive optics (KAPA) program. The program includes four key science projects, anupgrade to the Keck I laser guide star (LGS) adaptive optics (AO) facility to improve image quality and sky coverage, AO telemetry based PSF estimates for allscience exposures, and an educational component focused on broadening the participation of women and underrepresented groups in instrumentation. Allof these elements have pathfinder relevance for the ELTs. For the purpose of this conference we will focus on the AO facility upgrade which includesimplementation of a new laser, wavefront sensor and real-time controller to support laser tomography, the laser tomography system itself, andmodifications to an existing near-infrared tip-tilt sensor to support multiple NGS tip-tilt and focus measurements.
KAPA TeamTechnical Team1: K. Casey, J. Chin (Proj. Manager), S. Cetre,C. Correia, S. Lilley, S. Ragland, E. Wetherell, P Wizinowich (PI)Science Team: A. Ghez (Science Legacy Lead)4, M. Liu5,J. Lu (Proj. Scientist)3, D. Mawet6, C. Max2, M. Morris4, T. Treu4,S. Wright7
Education Lead: L. Hunter2
1WMKO, 2UCSC, 3UCB, 4UCLA, 5UH, 6Caltech, 7UCSD
Technical Collaborators: C. Boyer, A. Bouchez, S. Esposito, T. Fusco, J.-P. VeranConsultant: M. van DamLaser: TOPTICA Photonics & MPB Communications RTC: Microgate, Swinburne University of Technology, Australian National University, Observatoire de Paris
90 k
m
Laser Tomography (3 LGS asterism)
• Asterism generator with a beam splitterassembly to provide 3 LGS
• 6.4" radius beam separation• Field rotation is provided• Individual closed loop tip/tilt control from
wavefront sensor• 3 LGS spots on single OCAM2k camera
detector• Operational scenarios on WFS
• Single NGS/LGS centered on the opticalaxis, centered on the detector
• Three LGS beams separated by 120°,offset from reducer optics optical axis by1.691mm.
Pupils on lenslet array
1. Constraining dark matter, the Hubble constant, and dark energy via strong gravitational lensing 2. Testing General Relativity and studying supermassive black hole interactions at the Galactic Center3. Characterizing galaxy kinematics and metallicity using rare highly magnified galaxies4. Directly studying gas-giant protoplanets around the youngest stars
Performance Improvements
Science Case Publicly Available Data ProductsDark Matter Subhalo mass functionDark Energy Stellar velocity fields
Kinematics catalogReference frameStellar spectral & photometric properties Internal kinematics of lensed galaxiesMetallicity gradients of lensed galaxiesContrast curvesList of identified candidatesImaging data
Galactic Center
Galaxy Evolution
Gas-Giant Protoplanets
Key Science Programs
Akamai
AstroTech
KVS
Postdocs
Undergrad
Grad
Postdoc
Broaden participation in instru
mentation for women & URM
Educational Program and Outreach
ACKNOWLEDGEMENTS• The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
• Funding support for the KAPA System provided by the National Science Foundation Mid Scale Innovations Program award AST-1836016.
• Funding support for the AstroTech instrumentation intensive provided by the Heising-Simons Foundation.
• Keck II RTC is funded by the NSF Major Research for Instrumentation Program award AST-1727071• The authors wish to recognize and acknowledge the very significant cultural role and reverence that
the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
• Photos: Courtesy of Ethan Tweedie, TOPTICA, and WMKO staff
Project ElementsLaser Laser
Tomography
K1 RTC Upgrade
NIR Tip-tilt Upgrade
PSF-R for OSIRIS
KAPA Science
K2 RTC Upgrade
Education/Outreach
Real Time Controller
(Microgate)
• Microgate is collaborating with Swinburne University, Australian National University, Observatoire de Paris to provide RTC
• GPU based RTC with telemetry recorder storage (100TB); based on Keck II RTC Upgrade funded by NSF Major Research Instrumentation Program
• Dedicated FPGA hardware to interface with existing and new AO sensors, and motion devices: pyramid WFS, SH WFS, downlink and uplink tip-tilt mirrors , IR-TT and visible TT sensors, MEMS and piezo DMs
• FPGA based uXLink interface board to reduce jitter with direct DMA transfer of data into the GPUs; based on European Green Flash Project
• Flexible architecture to add future hardware, modes and capabilities: sensor fusion, predictive control, PSF-R
• CACAO (compute and control for AO) libraries for low latency processing; CACAO currently operating on PWS as a prototype
• OCAM2K EMCCD WFS for 3 LGS on a single detector• Initial performance demonstrates <100us latency• Built-in simulator
PSF-R with OSIRIS InstrumentNIR Tip-tilt Upgrade
102″102″
• Upgrade existing sensor to use 3 NGS for tip-tilt
• Reduces tip-tilt anisoplanatism• Implement LIFT algorithm to also provide
focus
• Replacement of solid state laser with aTOPTICA/MPBC fiber laser for improvedreliability and sodium return
• Integrate laser with existing CenterLaunch System
• Upgrade Software Sequencer Control
TOPTICA Laser and Center Launch Beam Train
• PSF-Reconstruction (PSF-R) using AO telemetry, atmospheric profile and instrument characterization
• Science data and PSF-R archived in Keck Observatory Archive.• Will port on-axis algorithms developed for NIRC2 after science
verification• Development of OTF terms for tomography
TRICK Dewar and Electronics
Photo Courtesy of TOPTICA
Photo Courtesy of WMKO
AstroTech Development Workshop, July 15-19 at UCB
Photo Courtesy of WMKO
Photo Courtesy of WMKO
Photo Courtesy of WMKO
