J. L. Margot, P. A. Taylor, M. Nolan, E. Howell, S. J. Ostro, L. A. M. Benner, J. D. Giorgini, C. Magri, L. Carter
Observations of 2000 DP107 in 2008 provide an exceptional opportunity to characterize the dynamics, morphology, and physical properties of a binary (or multiple) system. High resolution images obtained over a suitable range of aspect angles will provide detailed information on the regolith, size, shape, and spin of the components and on their mutual orbit and dynamical interactions.
In conjunction with pre-existing observations, these data will probe the formation and evolution of binaries in great detail, including dynamical processes such as tidal interactions and tumbling, radiative processes such as YORP, and erosional processes such as avalanches and lofting/redeposition of material. The signal-to-noise ratio will exceed 200 per run, allowing high quality images to be obtained.
UT Date RTT DEC UT rise-set runs SNR/run ----------------------------------------------------------- 2008 SEP 10 57.8 3 10:17-11:52 49 229 2008 SEP 11 57.8 5 09:43-11:41 61 229 2008 SEP 13 59.2 10 08:43-11:08 73 210 2008 SEP 15 62.6 15 07:53-10:31 76 174 2008 SEP 18 70.5 20 06:50-09:33 69 115 2008 SEP 21 81.1 23 06:00-08:40 59 71 2008 SEP 24 93.6 25 05:18-07:55 50 43
DOY UT date --- UT window --- 253 2008 SEP 09 0900 1030 1545 1615 254 2008 SEP 10 0830 1000 1550 1620 256 2008 SEP 12 0810 0940 1500 1530 257 2008 SEP 13 0735 0905 1315 1345 258 2008 SEP 14 0750 0920 1450 1520
Goldstone pointing macros:
UT RA DEC dRA dDEC
(deg) (deg) (mdeg) (mdeg)
2008 SEP 09 10:00 94.210 -0.0994 3.3 1.8
2008 SEP 09 13:00 93.599 0.2328 3.4 1.8
2008 SEP 09 16:00 92.977 0.5661 3.4 1.8
2008 SEP 10 10:00 89.416 2.5805 3.3 1.8
2008 SEP 10 13:00 88.792 2.9186 3.4 1.8
2008 SEP 10 16:00 88.160 3.2558 3.4 1.8
2008 SEP 12 09:00 79.906 7.7968 3.3 1.8
2008 SEP 12 12:00 79.284 8.1221 3.4 1.7
2008 SEP 12 15:00 78.654 8.4429 3.3 1.7
2008 SEP 13 08:00 75.306 10.2136 3.3 1.7
2008 SEP 13 11:00 74.698 10.5224 3.4 1.7
2008 SEP 13 14:00 74.080 10.8256 3.5 1.7
2008 SEP 14 09:00 70.420 12.6686 3.2 1.6
2008 SEP 14 12:00 69.824 12.9521 3.3 1.6
2008 SEP 14 15:00 69.226 13.2279 3.4 1.5
/share/obs4/usr/radar/2000DP107Data reduction scripts are stored in :
/proj/radar/2000DP107
Ephemerides are available in:
/share/trabuco4/jplephem/osod/ops/a185851 aardvark:/export/data3/osod/ops/a185851Jon prepared solution 85. If Goldstone observations are successful on September 9, we should get a range measurement, which we'll use to create a solution that should remain valid throughout the campaign.
Relevant 3-sigma uncertainties from Jon Giorgini are listed below:
Solution 85 Date__(UT)__HR:MN POS_3sigma DOP_S-sig DOP_X-sig RT_delay-sig 2008-Sep-09 00:00 4.50180357 0.23 0.83 0.001250 2008-Sep-11 00:00 3.57967510 0.11 0.39 0.001467 2008-Sep-13 00:00 2.49757193 0.10 0.36 0.001612 Solution 89 Date__(UT)__HR:MN POS_3sigma DOP_S-sig DOP_X-sig RT_delay-sig 2008-Sep-09 00:00 .509023188 0.10 0.37 0.000007 2008-Sep-11 00:00 .484947352 0.09 0.31 0.000018 2008-Sep-13 00:00 .435579406 0.07 0.24 0.000037 2008-Sep-15 00:00 .374295491 0.05 0.17 0.000052 2008-Sep-17 00:00 .316579045 0.03 0.11 0.000061 2008-Sep-19 00:00 .271869535 0.02 0.09 0.000065 2008-Sep-21 00:00 .242056311 0.03 0.10 0.000066
The secondary is likely ~300 m in diameter and spins with ~42 hours period (Margot et al., 2002), so the limb-to-limb bandwidth will be 0.2 S-band Hz. Because the round-trip time always exceeds 50 seconds, we should be able to place at least 10 resolution elements on the secondary in the Doppler dimension.
1. Start with a few CW runs to confirm detection.
2. Obtain ranging runs for unambiguous range detection (10 and 11 usec with 127-length codes).
3. Update ephemeris.
4. Obtain imaging runs (1 us baud, 8191 code, 122 Hz bandwidth, 5 or 10 Hz tx offset)
5. End with a few CW runs.
1. Start with a few CW runs to confirm detection.
2. Switch to high resolution (0.2 us) imaging setup.
3. End with a few CW runs.
1. Start with ten CW runs to confirm detection.
2. Obtain imaging data at 0.5 us baud (0.5 us baud, 8191 code, 244 Hz bandwidth, 5 or 10 Hz tx offset)
3. End with ten CW runs.
1. Start with 10 CW runs to confirm detection.
2. Obtain imaging runs (1 us baud, 8191 code, 122 Hz bandwidth, 5 or 10 Hz tx offset)
3. Intersperse boresights if pointing is in question.
4. End with 10 CW runs.
1. Start with 10 CW runs to confirm detection.
2. Obtain imaging runs (2 us baud, 4095 code, 122 Hz bandwidth, 5 or 10 Hz tx offset)
3. Intersperse boresights if pointing is in question.
4. End with 10 CW runs.
1. Start with a few CW runs to confirm detection.
2. Switch to high resolution (0.2 us) imaging setup. Sample at 10 MHz with PFS, no matched filters.
3. End with a few CW runs.
1. Start with a few CW runs to confirm detection.
2. Switch to moderate resolution (0.5 us) imaging setup.
3. End with a few CW runs.
Name Institution Work phone Cell phone Email
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PI Jean-Luc Margot Cornell 607 255 1810 607 229 5015 jlm@astro.cornell.edu
Rising star Patrick Taylor Cornell 607 255 2727 ptaylor@astro.cornell.edu
AO guru/friend Mike Nolan NAIC 787 878 2612 x 334 nolan@naic.edu
DSN guru/friend Lance Benner JPL 818 354 7412 626 319 4369 lance.benner@jpl.nasa.gov
TX clearance Reid Drummond GDSCC 760 255 8218 rdrummond@jgld.gdscc.nasa.gov
TX clearance Larry Sturgis GDSCC 760 255 8071 LSturgis@jgld.gdscc.nasa.gov
DSN operator J. Van Brimmer RARG/ADVDEV 760 255 8469 JVanbrimmer@gdscc.nasa.gov
DSN operator M. Silva RARG/ADVDEV 760 255 8469 masilva@gdscc.nasa.gov
DSN L. Juare RARG/ADVDEV 760 255 8469 LJuare@gdscc.nasa.gov
Ephemerides Jon Giorgini JPL 818 393 3107 jdg@tycho.jpl.nasa.gov
GSSR support Joseph Jao JPL 818 354 2102 818 640 5802 Joseph.S.Jao@jpl.nasa.gov
Patrick VSQ 787 878 2612 x 379 JPL radar central 818 354 2877 Goldstone Pedestal 760 255 8470,8469,8259
Return to my home page.
jlm@astro.cornell.edu