Physical and dynamical properties of the main belt triple asteroid (87) Sylvia

We present the analysis of high angular resolution observations of the triple asteroid (87) Sylvia collected with three 8–10 m class telescopes (Keck, VLT, Gemini North) and the Hubble Space Telescope. The moons’ mutual orbits were derived individually using a purely Keplerian model. We computed the position of Romulus, the outer moon of the system, at the epoch of a recent stellar occultation which was successfully observed at less than 15 km from our predicted position, within the uncertainty of our model. The occultation data revealed that the moon, with a surface-area equivalent diameter DS = 23.1± 0.7 km, is strongly elongated (axes ratio of 2.7± 0.3), significantly more than single asteroids of similar size in the main-belt. We concluded that its shape is probably affected by the tides from the primary. A new shape model of the primary was calculated combining adaptive-optics observations with this occultation and 40 archived light-curves recorded since 1978. The difference between the J2 = 0.024 +0.016 −0.009 derived from the 3-D shape model assuming an homogeneous distribution of mass for the volume equivalent diameter DV = Based on observations collected at the European Southern Observatory, Paranal, Chile (089.C-0944, 087.C-0014, 385.C-0089, 085.C-0480, 077.C-0422, 074.C-0052), at the Gemini North Observatory in Hawaii, and at the W. M. Keck Observatory. The Keck observatory was made possible by the generous financial support of the W. M. Keck Foundation. Corresponding author Email address: [email protected] (J. Berthier) Preprint submitted to Elsevier July 4, 2014 273± 10 km primary and the null J2 implied by the keplerian orbits suggests a non-homogeneous mass distribution in the asteroid’s interior.