PALM-3000 Observers Information - 2011B

Overview

PALM-3000 and its back-end instruments are optimized for high-angular resolution science at visible and near-infrared wavelengths. As the world's highest order adaptive optics system, PALM-3000 will correct for atmospheric turbulence to an unprecedented degree using a new 3,388 actuator deformable mirror in conjunction with the former 349 actuator

2011B Call for Proposals

PALM-3000 will be available for shared-risk science observations, per the Call for Proposals [add ref. link here], in 2011B.

Current Instrument Status

PALM-3000 is undergoing system integration at Palomar Observatory. We expect our first light engineering test of PALM-3000 in mid-May 2011.
PHARO is currently operational at the summit and we expect to open the dewar for a single mask/filter exchange in late-April 2011.
P1640 - coronagraph + CAL is undergoing integration and testing at JPL in Pasadena.
P1640 - IFS is enjoying an upgrade to a science-grade H2RG detector at AMNH in New York City.
SWIFT is currently undergoing refurbishment at Oxford University, UK.

Expected System Capabilities

For 2011B, PALM-3000 will support natural guide star wavefront sensing (only) in the following correction modes:

Number of subapertures per pupil diameter	Limiting magnitude	Best performance magnitude	Notes
62	V ~ 7	V < 5.5
32	V ~ 10	5.5 < V < 7.5

Expected Performance

PALM-3000 Error Budget Summary

[check back here for a plot of expected performance]

Expected Performance vs. Seeing

Expected Observing Overheads

Expected AO overheads: These numbers reflect performance as of May 2005. AO & laser startup (from 12° twilight) 30 min Acquisition of new target (TT ref. R<15.5) 3-5 min Acquisition of new target (TT ref. 15.5 < R < 17.0) 5-8 min Acquisition of new target (TT ref. R>17.0) 6-10 min Dither with laser move 20 sec Dither without laser move 10 sec Recovery from aircraft or LTCS shuttering of the laser 3 min

Last updated - 03 Mar 2011

Topic revision: r1 - 2011-03-03 - RichardDekany

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