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Future Opportunities for Adaptive Optics Galactic Science

Future Opportunities for Adaptive Optics Galactic Science. Andrea Ghez University of California Los Angeles. Targets/Science. Young Stars Direct detection of planets Dynamical measurements of low mass binaries (calibrate pre-main sequence evolutionary tracks) Circumstellar Disks

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Future Opportunities for Adaptive Optics Galactic Science

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  1. Future Opportunities for Adaptive Optics Galactic Science Andrea Ghez University of California Los Angeles

  2. Targets/Science • Young Stars • Direct detection of planets • Dynamical measurements of low mass binaries (calibrate pre-main sequence evolutionary tracks) • Circumstellar Disks • Grain growth • Structure induced by young planets • Embedded Young Objects • Envelope/Disk structure • Evolved Stars • Mass loss • Globular Clusters • Dynamical measurements (astrometric and spectroscopic) to search for intermediate mass black holes • Photometric measurements to study stellar population • Galactic Center • Dynamical measurements (astrometric and spectroscopic) to search for extended dark matter & Ro • Spectroscopy - stellar population and dynamics

  3. Much of this Science Benefits From High Strehl Over Small/Modest FOV • Strehls at 3.8 mm: S= 0.5 – 0.7 • ~2 hour on-source integration using NIRC2/AO. • Peak disk = 1/2750 of GG Tau A peak

  4. For Grain Growth Studies Need High Strehl Over Large Wavelength Range & Polarimetry =amax 0.3mm 0.5mm 0.9mm 1.25 mm 1.5 mm WFPC2 F814W NICMOS F110W NICMOS F160W NIRC2 L' Observations Models

  5. Many of These Object are Very Red - How Can we Compete With the IR WFS at VLT? Note: SIFONI has optical WFS First spectrum of Sgr A*? First direct detection of a giant planet?

  6. How Much Would an IR TT Sensor Help the LGS vs. an IR-WFS? 5” LGS Strehls under great conditions, 0.35 (K) and 0.7 (L’) Guide Stars: (1) K = 7 mag at 5”, (2) R = 13.2 mag at 30” (3) 13.7 mag at 20”

  7. External Fund Raising Opportunity at UCLA if there is a Route to Improve GC observations • Moore Foundation • Originally approached last fall by UCLA for Center for IR, now considering IR-WFS proposal • UCLA • Funds from Dean • Development Office interested • VC Research (Roberto Peccei) also offered help • But how best to match this with a strategic plan

  8. Would an IR TT/WFS Help the building Pressure on Grey Time? • Our current AO systems are moving a community that traditionally requests bright time to gray time

  9. Conclusions • There are lots of great AO targets within our Galaxy • Need to figure our how to make LGS more available (and robust) • Most benefit from high strehl performance over small/modest fields of view • Increasing wavelength range and adding polarimetry will benefit some studies (e.g., grain growth) • Visible AO • Thermal IR (3-5 micron) optimized AO system • IR TT/WFS offers advantage for dusty targets (YSO, Mass Loss, GC) • Fund raising opportunity at UCLA for GC observations • Reduces pressure on grey time

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