2 research outputs found
A Single-chord Stellar Occultation by the Extreme Trans-Neptunian Object (541132) Leleākūhonua
A stellar occultation by the extreme large-perihelion trans-Neptunian object (541132) Leleākūhonua (also known by the provisional designation of 2015 TG387) was predicted by the Lucky Star project and observed with the Research and Education Collaborative Occultation Network on 2018 October 20 UT. A single detection and a nearby nondetection provide constraints for the size and albedo. When a circular profile is assumed, the radius is r = 110+14-10 km, corresponding to a geometric albedo Pv = 0.21+0.03-0.05, for an adopted absolute magnitude of HV = 5.6, typical of other objects in dynamically similar orbits. The occultation also provides a high-precision astrometric constraint
The Sizes and Albedos of Centaurs 2014 YY and 2013 NL from Stellar Occultation Measurements by RECON
In 2019, the Research and Education Collaborative Occultation Network (RECON)
obtained multiple-chord occultation measurements of two centaur objects: 2014
YY on 2019 January 28 and 2013 NL on 2019 September 4. RECON is a
citizen-science telescope network designed to observe high-uncertainty
occultations by outer solar system objects. Adopting circular models for the
object profiles, we derive a radius km and a geometric albedo
for 2014 YY, and a radius km and geometric albedo for 2013
NL. To the precision of these measurements, no atmosphere or rings are
detected for either object. The two objects measured here are among the
smallest distant objects measured with the stellar occultation technique. In
addition to these geometric constraints, the occultation measurements provide
astrometric constraints for these two centaurs at a higher precision than has
been feasible by direct imaging. To supplement the occultation results, we also
present an analysis of color photometry from the Pan-STARRS surveys to
constrain the rotational light curve amplitudes and spectral colors of these
two centaurs. We recommend that future work focus on photometry to more
deliberately constrain the objects' colors and light curve amplitudes, and on
follow-on occultation efforts informed by this astrometry