(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body
Creators: name: Hanuš, J.
name: Vernazza, P.
name: Viikinkoski, M.
name: Ferrais, M.
name: Rambaux, N.
name: Podlewska-Gaca, E.
name: Drouard, A.
name: Jorda, L.
name: Jehin, E.
name: Carry, B.
name: Marsset, M.
name: Marchis, F.
name: Warner, B.
name: Behrend, R.
name: Asenjo, V.
name: Berger, N.
name: Bronikowska, M.
name: Brothers, T.
name: Charbonnel, S.
name: Colazo, C.
name: Coliac, J-F.
name: Duffard, R.
name: Jones, A.
name: Leroy, A.
name: Marciniak, A.
name: Melia, R.
name: Molina, D.
name: Nadolny, J.
name: Person, M.
name: Pejcha, O.
name: Riemis, H.
name: Shappee, B.
name: Sobkowiak, K.
name: Soldán, F.
name: Suys, D.
name: Szakats, R.
name: Vantomme, J.
name: Birlan, M.
name: Berthier, J.
name: Bartczak, P.
name: Dumas, C.
name: Dudziński, G.
name: Ďurech, J.
name: Castillo-Rogez, J.
name: Cipriani, F.
name: Fetick, R.
name: Fusco, T.
name: Grice, J.
name: Kaasalainen, M.
name: Kryszczynska, A.
name: Lamy, P.
name: Michalowski, T.
name: Michel, P.
name: Santana-Ros, T.
name: Tanga, P.
name: Vachier, F.
name: Vigan, A.
name: Witasse, O.
name: Yang, B.
Publisher: name: arXiv
Year: 2019
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: With an estimated diameter in the 320 to 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with $D$ &gt; 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with $D$ $\lesssim$ 200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller ($D$ $\lesssim$ 200 km) bodies. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling (ADAM) algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Interamnia's volume-equivalent diameter of 332 $\pm$ 6 km implies a bulk density of $ρ$=1.98 $\pm$ 0.68 gcm$^{-3}$ , which suggests that Interamnia - like Ceres and Hygiea - contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2 $σ$ level. The rather regular shape of Interamnia implies that the size and mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller ($D$ $\lesssim$ 300km) less massive ($m$ $\lesssim$ 3x10$^{19}$ kg) bodies.
description: Accepted for publication in Astronomy and Astrophysics