(r20) ProposerInfo < Palomar/Palm3000

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---+ PALM-3000 Observers Information - 2014A

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---++ 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 corrects for atmospheric turbulence to an unprecedented degree using a new 3,388 actuator Xinetics deformable mirror in conjunction with the former 349 actuator Xinetics DM and separate fast tip-tilt mirror.  Wavefront sensing requires a bright natural guide star in proximity to the science target.

---++ 2014A Call for Proposals
PALM-3000 will be available for PHARO science, shared-risk SWIFT science, and private instrument observations in 2014A. 
   * [[http://www.astro.caltech.edu/observatories/coo/solicit][Detailed COO Call for Proposals]]

---++ Instruments Status
   * PALM-3000 is operational and working through a period of performance optimization.  Wavefront correction to date has demonstrated performance in the range of 150-160 nm RMS wavefront error (equivalent to peak K-Strehl = 82%), which is not yet at the ultimate expected performance level of 105 nm RMS (the 105nm requirement is for a V = 5 guide star (in median seeing conditions).  

The current performance of 160nm RMS has been demonstrated with V = 8 guide stars, which however does approximately meets the design specification.  Certain wavefront sensor camera issues are currently suspected of limiting performance on brightest stars (operating AO at fastest frame rates), and are under active investigation.

   * Instrument Status:
      * PHARO (public)
         * Is currently operational at the summit.
      * SWIFT (public)
         * Is performing routine science in both AO-fed and AO-passthrough (seeing-limited) operation.
      * P1640 (private, PI: B. Oppenheimer, AMNH)
         * Coronagraph + CAL is performing routine science in a large exoplanet imaging and spectroscopic survey.
      * Fiber Nuller (private; PI: G. Serabyn, JPL)
         * Initial FN tests with PALM-3000 successful in June 2012.  
      * TMAS (private; co-I's: R. Dekany and S. Hildebrandt, COO)
         * First light successful 27 Sept 2012.  Strategies for improving sensor quality are under investigation.  Science observations in 2013B.
      * DARKNESS (private; PI: B. Mazin, UCSB)
         * Development of energy-resolving MKIDS technology imager funded by NSF in Summer 2013.  First light schedule is TBD.

---++ Measured Performance vs. NGS Brightness
   * s64 pupil sampling mode: Small (8.3cm) subapertures
      * We show below the !P3K+PHARO K-band Strehl ratio obtained in June 2012, September 2012, and March 2013 taken in a variety of seeing conditions over 6 nights.  The data clearly show the progression of instrument performance from 2011 to present, especially on bright guide stars.  No consistent optimization of frame rate for each guide star was attempted for these data sets (we were doing other engineering and not specifically exploring the frame rate parameter space).  We intend a more rigorous strehl investigation on bright to faint stars in May 2013.
   * s32 pupil sampling mode: Larger (16.2 cm) subapertures
      * We have successfully commissioned the 32x pupil sampling mode during our engineering night on March 22, 2013.  The Palomar staff can now operate P3K in both 64x and 32x pupil sampling modes.  
      * Based on expected P3K performance and our experience on a few targets on March 22 (see figure below), we suggest using 64x mode on targets brighter than 12 mv if the visible seeing is at or better than 1.0".  For target stars fainter than 9 mv in visible seeing greater than 1.0", 32x mode may perform better than 64x.  The Palomar staff can help you determine which mode may be best given the local conditions.
      * 32x did out-perform 64x on 11.5 and 13 mv target stars on the night of March 22 in 15-20 mph surface winds and variable seeing conditions (1.0-1.7 Ksh seeing).
   * s8 pupil sampling mode: Largest (65 cm) subapertures
      * Will NOT be available until 2014 at the earliest
   * Performance optimizations are on-going through FY14.
<img src="%ATTACHURLPATH%/p3k_Ksh_strehl.png" alt="1108_P3k_S64_StrehlPerf.jpg" width='721' height='451' />

---++ Expected System Capabilities 
For 2014A, PALM-3000 will support natural guide star wavefront sensing (only) in the following correction modes:

| Number of subapertures per pupil diameter | WFS limiting mag | WFS best performance mag |  Notes  |
|  64  |  V < 11  |  V < 7  | |
|  32  |  V < 13  |  V < 10  | |
|  8  |  V < 17  |  ---  | No sooner than 2014B|
|  16  |  V < 14  |  ---  | Not currently planned due to funding constraints |

PALM-3000 correction will be best in the direction of the guide star, and fall off due to atmospheric anisoplanatism.  The corrected field of view diameter will vary with conditions, but is generally expected to be between 1-2 arcmin diameter in K-band, decreasing to 10-20 arcsec in I-band.

---++ Guide Star Selection

PALM-3000 has a patrol range for NGS selection of ~90 arcsecond in diameter (allowing a guide star up to 90" away from the science target to be utilized, with the understanding that anisoplanatism error (not accounted for in any data elsewhere on this page) degrades performance significantly beyond ~30 arc sec radius in H/K bands (and beyond ~15 arc sec in Y/J bands.)

The WFS acquisition camera FOV is ~ 95 arc sec x 80 arc sec (TBC).

---++ Ultimate Expected Performance on Bright Guide Stars

The bright star wavefront error budget for PALM-3000  is as follows:

* Assumptions
   * Mean turbulence weighted wind speed = 9.5 m/s
   * Zenith pointing
   * Guide star brightness V ~ 5
   * AO mode: s64

|  Seeing  |  r_0(0.5um)  | RMS residual wavefront error |  Strehl Ratio  ||||||| Notes |
| | | | r' | i' | Z | Y | J | H | K | |
| | | | 0.62um | 0.75um | .88um | 1.03um | 1.25um | 1.64um | 2.2um ||
|  0.7"  |  0.14 m  |  83 nm  |  48%  |  61%  | 70%  |  78%  |  84%  |  90%  |  95%  | Variations in non-common-path errors may limit PHARO K Strehl to ~90% even in excellent seeing |
|  1.1" (median)  |  0.092 m  |  105 nm  |  32%  |  46%  |  57%  |  66%  |  76%  |  85%  |  91% | See above |
|  1.6"  |  0.07 m  |  165 nm  |  26%  |  38%  | 47%  |  54%  |  61%  |  68%  |  73%  | - |

---++ Expected Observing Overheads
Instrument requirement #0480 states that PALM-3000 shall be ready to begin a science exposure < 2 minutes after the end of a telescope slew (< 1 minute goal).  During shared-risk science observing in 2012A, we expect observations performed in a single AO mode in a localized part of the sky to approach the final requirement. For now, changes in telescope pointing or AO mode may result in greater acquisition overheads.

Closed-loop AO image dithering on PHARO is expected to be functional at a level equal to or better than the prior PALMAO system (smallest step size ~ 5 mas), with improved non-common-path flexure during long exposures.  Early engineering tests confirm PALM-3000 has improved flexure stability compared to PALMAO.  These results are being quantified.

---++ Wide-field astrometry
We do not recommend precision wide-field PHARO astrometric programs, due to the uncharacterized nature of our dual-DM-conjugate correction architecture.  Contact the PALM-3000 PI for further details.

---++ Extended objects
PALM-3000 is designed to support NGS observations of Uranus and Neptune, but optimization on these targets will require additional calibration effort.  To date, in S64 mode, good correction has been obtained locking on Saturn's moon Titan (V~8 and diameter ~ 1").  Contact the PALM-3000 PI for further information.

---++ Contact information
Technical inquiries for specific observing proposals not addressed here can be referred to Principal Investigator Richard Dekany at Caltech Optical Observatories or Rick Burruss at JPL.

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Last updated - 03 September 2013 - R. Dekany<br>

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I	Attachment	History	Action	Size	Date	Who
jpg	1108_P3k_S64_StrehlPerf.jpg	r1	manage	66.4 K	2012-03-08 - 18:48	RichardDekany
png	p3k_Ksh_strehl.png	r1	manage	98.6 K	2013-03-29 - 21:53	RickBurruss
png	p3k_strehl_20121106.png	r1	manage	100.2 K	2012-11-06 - 20:30	RickBurruss
Topic revision: r20 - 2013-09-03 - RichardDekany
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