This table lists the best candidates for TNO occultation for the next two years that are visible from the entire network. These events all have a minimum success probability of 30%.
This list was last updated at 2017/06/23 16:01:43 UT
|Idx||ET||Desig||Diam(5%)||Diam(30%)||DES Classification||TNO pos err||StarID||RA||Dec||mag||minsep||selong||RECON||Prob|
|84861||2017 Oct 26 09:12:58||13WV107||57||23||CENTAURR||0.17||UC4-543-040693||07:15:53.9||+18:28:30||16.1||0.10||105||1.00||69.9%|
|94685||2017 Dec 11 08:02:07||15875||240||98||3:2E||1.14||UC4-591-018990||05:28:00.4||+28:00:52||16.3||0.11||174||1.00||38.5%|
|153164||2018 Sep 12 11:25:44||10TH||88||36||CENTAURR||0.09||UC4-471-011981||05:33:36.8||+04:01:44||16.0||0.12||87||1.00||34.4%|
|179173||2019 Jan 28 05:11:20||14YY49||58||24||CENTAURR||0.14||UC4-458-028181||06:59:55.5||+01:25:26||14.6||0.27||150||1.00||38.5%|
The green lines highlight those events for which the star is visible to the entire RECON network at the time of the appulse. This corresponds to a "score" (second to last column) of 1. If the score is between 0 and 1, only part of the network can view the star at the right time. The last column is the estimate of the probability of success for RECON if it attempts this event. This number is based on the uncertainty in the prediction combined with the actual geometry for RECON for the event. In general, we look for a probability greater than about 30% for an official RECON campaign. This probability does not include any factors such as weather.
Most of the columns are self-explanatory. The two diameters give an estimate of the size of the object for two different albedos (5% and 30%). "TNO pos err" is the uncertainty in the position of the TNO at the time of the appulse, in arc-seconds. An additional uncertainty of 0.05 arcsec is assumed for the uncertainty in the star position. "minsep" is the minimum separation (in arcsec) between the star and TNO as seen from the position of the center of the earth. "selong" is the angle between the sun and the object (solar elongation) at the time of the event.Marc W. Buie, Southwest Research Institute