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W. M. Keck Observatory’s Next Generation Adaptive Optics (NGAO) Facility

W. M. Keck Observatory’s Next Generation Adaptive Optics (NGAO) Facility. Peter Wizinowich, Sean Adkins, Rich Dekany, Don Gavel, Claire Max for NGAO Team: R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Kupke, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Neyman,

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W. M. Keck Observatory’s Next Generation Adaptive Optics (NGAO) Facility

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  1. W. M. Keck Observatory’sNext Generation Adaptive Optics(NGAO) Facility Peter Wizinowich, Sean Adkins, Rich Dekany, Don Gavel, Claire Max for NGAO Team: R. Bartos, J. Chin, A. Conrad, A. Delacroix, R. Kupke, C. Lockwood, J. Lyke, E. McGrath, D. Medeiros, D. Morrison, C. Neyman, S. Panteleev, C. Pollard, M. Reinig, T. Stalcup, S. Thomas, M. Troy, K. Tsubota, V. Velur, K. Wallace, E. Wetherell SPIE, San Diego June 28, 2010

  2. Context for NGAO – growing demand for LGS-AO on large telescopes ~270 Keck AO science papers ~50% of Keck II science nights Credit: M. Liu 2

  3. NGAO - Next Generation AO Key Science Goals Understanding the Formation and Evolution of Today’s Galaxies since z=3 Measuring Dark Matter in our Galaxy and Beyond Testing the Theory of General Relativity in the Galactic Center Understanding the Formation of Planetary Systems around Nearby Stars Exploring the Origins of Our Solar System Key New Science Capabilities Near Diffraction-Limited in Near-IR (K-Strehl ~80%) AO correction at Red Wavelengths (0.7-1.0 m) Increased Sky Coverage Improved Angular Resolution, Sensitivity and Contrast Improved Photometric and Astrometric Accuracy Imaging and Integral Field Spectroscopy

  4. Flowed-Down Key Architectural Features

  5. NGAO System Architecture • Key Features: • Fixed narrow field laser tomography • AO corrected NIR TT sensors • Cooled AO enclosure • Cascaded relay • Combined imager/IFU instrument

  6. NGAO: AO Layout 6

  7. NGAO: AO Bench 7

  8. LGS Wavefront Sensor Assembly 8

  9. Low Order Wavefront Sensor Assembly

  10. Imager detector head Pupil imager wheel Grating selector wheel IFS detector head Imager/IFS selector mirror Filter and pupil mask wheels Coronagraph mask wheel Entrance window DAVINCI – Imager & IFS • On axis imager 28.7" x 28.7" FOV • 7 mas pixel scale • On axis selectable IFS • 50 mas pixel scale FOV 5.6" x 3" • 35 mas, FOV 3.92" x 2.1" • 10 mas, FOV 1.12" x 0.6" Adkins et al. 7735-287

  11. AO Enclosure DM Electronics DAVINCI Instrument AO Bench LGSWFS Interferometer DSM Gowning Room Area Secondary Instrument Thermal Management Overhead HEPAs

  12. LGS Facility RC Optical TOPTICA/MPBC 7736-252

  13. Control Loops – LGS AO Example

  14. Control Loops – LGS AO Example

  15. Control Loops – LGS AO Example

  16. Control Loops – LGS AO Example

  17. Control Loops – LGS AO Example

  18. Control Loops – LGS AO Example

  19. The RTC System Architecture is Mapped to the Critical Signal Paths TT Star Sharpenning Reinig & Gavel 7736-130 Tip/Tilt Tomography At the heart of the science wavefront control is the Tomography Engine 19

  20. Science Case Performance Summary Galaxy assembly: 30º zenith angle, 60º galactic latitude, 30 min integ. 20

  21. NGAO Performance vs. Sky Coverage (Galaxy Assembly Science Case) Strehl EE 70 mas EE 50 mas EE 35 mas Resid. TT error • Nominal Ensquared Energy (EE) requirement = 30% sky coverage • But very little degradation in EE even for 70% sky coverage 21

  22. NGAO is robust against conditions and design assumptions 22

  23. NGAO changes the 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%) 23

  24. Early Science Benefits from NGAO - 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

  25. 1% photometry Keck II Center Launch + New LaserPredicted Performance for T Dwarf Binary Case Factor of 2x improvement  6x in dynamical mass determination R = 16.2 NGS 31” off-axis 50 zenith angle

  26. Early Science Benefits from NGAO - 2 • PSF reconstruction • Collaboration with Gemini & U. Groningen to demonstrate on-axis NGS AO PSF reconstruction on Gemini & Keck Jolissaint et al., 7736-50 • 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

  27. NIR Tip-Tilt SensorPredicted Performance for High Redshift Galaxies Case

  28. Chin 7736-66; LMCT -69 Major Keck AO Science Capability Milestones Future

  29. In Closing NGAO Keck AO • Keck AO has been delivering great science • NGAO will ensure cutting edge high angular resolution science for the US community NGAO PD funding from NSF/AURA TSIP

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