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A peculiar family of Jupiter Trojans: The Eurybates |
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| Authors: | F De Luise E Dotto MA Barucci D Perna F Marzari |
| Institution: | a INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monteporzio Catone (Roma), Italy b INAF - Osservatorio Astronomico di Collurania-Teramo, Via Mentore Maggini, s.n.c., 64100 Teramo (TE), Italy c LESIA, Paris Observatory, 5 Place Jules Janssen, 92195 Meudon Cedex, France d University of Paris VII “Denis Diderot”, 4 rue Elsa Morante, 75013 Paris, France e Fundación Galileo Galilei & Telescopio Nazionale Galileo, PO Box 565, 38700 S/C de La Palma, Tenerife, Spain f Oak Ridge Associated Universities (ORAU) - NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035-1000, USA g University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, 00133 Roma, Italy h Dipartimento di Fisica - University of Padova, Via Marzolo 8, 35131 Padova, Italy |
| Abstract: | The Eurybates family is a compact core inside the Menelaus clan, located in the L4 swarm of Jupiter Trojans. Fornasier et al. (Fornasier, S., Dotto, E., Hainaut, O., Marzari, F., Boehnhardt, H., De Luise, F., Barucci, M.A. 2007]. Icarus 190, 622-642) found that this family exhibits a peculiar abundance of spectrally flat objects, similar to Chiron-like Centaurs and C-type main belt asteroids. On the basis of the visible spectra available in literature, Eurybates family’s members seemed to be good candidates for having on their surfaces water/water ice or aqueous altered materials.To improve our knowledge of the surface composition of this peculiar family, we carried out an observational campaign at the Telescopio Nazionale Galileo (TNG), obtaining near-infrared spectra of 7 members. Our data show a surprisingly absence of any spectral feature referable to the presence of water, ices or aqueous altered materials on the surface of the observed objects. Models of the surface composition are attempted, evidencing that amorphous carbon seems to dominate the surface composition of the observed bodies and some amount of silicates (olivine) could be present. |
| Keywords: | Trojan asteroids Asteroids surface Asteroids composition Spectroscopy |
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