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A spectral comparison of (379) Huenna and its satellite
Authors:Francesca E DeMeo  Benoît Carry  Franck Marchis  Richard P Binzel  Schelte J Bus  Alin Nedelcu  Michael Busch
Institution:a Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
b LESIA, Observatoire de Paris, 5 Place Jules Janssen, 92195 Meudon Principal Cedex, France
c European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
d Université Paris 7 Denis-Diderot, 5 rue Thomas Mann, 75205 Paris Cedex, France
e University of California at Berkeley, Dept. Of Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA
f IMCCE, UMR8028 CNRS, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France
g Institute for Astronomy, 640 N. Aohoku Place, Hilo, HI 96720, USA
h Astronomical Institute of the Romanian Academy, 5 Cu?itul de Argint, RO-75212 Bucharest, Romania
i Department of Earth and Space Sciences, University of California Los Angeles, 595 Charles Young Dr. E., Los Angeles, CA 90095, USA
Abstract:We present near-infrared spectral measurements of Themis family Asteroid (379) Huenna (D ∼ 98 km) and its 6 km satellite using SpeX on the NASA IRTF. The companion was farther than 1.5″ from the primary at the time of observations and was approximately 5 magnitudes dimmer. We describe a method for separating and extracting the signal of a companion asteroid when the signal is not entirely resolved from the primary. The spectrum of (379) Huenna has a broad, shallow feature near 1 μm and a low slope, characteristic of C-type asteroids. The secondary’s spectrum is consistent with the taxonomic classification of C-complex or X-complex. The quality of the data was not sufficient to identify any subtle feature in the secondary’s spectrum.
Keywords:Asteroids  Spectroscopy
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