¹P. Beck, ¹B. Schmitt, ²E.A. Cloutis, ³P. Vernazza
¹Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France, CNRS, IPAG, F-38000 Grenoble, France
²Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, 6 Manitoba, Canada R3B 2E9
³Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France

The surface of Ceres, the most massive asteroid, presents a peculiar absorption band at 3.06 μm. This feature has been attributed to a number of candidate phases, including a magnesium hydroxide, brucite (Mg(OH)2). In order to gain insights into this possibility we have investigated the evolution of brucite reflectance spectrum under decreasing temperature (down to 93 K). Following early observation of brucite infrared spectra in transmission, a strong evolution of the reflectance spectrum of brucite is found under decreasing temperature. Small shifts of the band positions are found in particular at 1.36 and 1.39 μm, while the most important evolution is a decrease in intensity of the features at 2.82 and 3.06 μm. These observations can be seen in the light of the nature of these modes, which are transitions from excited states (difference bands) that are less populated under low-temperature. Such results provide a major test for the presence of brucite on Ceres from forthcoming DAWN observations, by searching for a possible evolution of the band with local time and then surface temperature. Based on the fact that the equivalent summation bands are not observed in Ceres spectra, brucite is not favored as the major constituent to the 3.06 μm feature. The possibility that this feature rather corresponds to ammoniated minerals (phyllosilicates or salts) is discussed.

Reference
Beck P, Schmitt B, Cloutis EA, Vernazza P (2015) Low-Temperature reflectance spectra of brucite and the primitive surface of 1-Ceres? Icarus (in Press)
Link to Article [doi:10.1016/j.icarus.2015.05.031]

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