Date post: | 19-Dec-2015 |
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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
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
Much of this Science Benefits From High Strehl Over
Small/Modest FOV
● Strehls at 3.8 m: S= 0.5 – 0.7●~2 hour on-source integration using NIRC2/AO.● Peak disk = 1/2750 of GG Tau A peak
For Grain Growth Studies Need High Strehl Over Large Wavelength Range & Polarimetry
WFPC2F814W
NICMOSF110W
NICMOSF160W
NIRC2L'
Observations Models
0.3m 1.5m1.25m0.9m0.5m =amax
Many of These Object are Very Red - How Can we Compete With the IR WFS at VLT?
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First direct detection of
a giant planet?
Note: SIFONI has optical WFSFirst spectrum of Sgr A*?
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”
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
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
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