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By Allington-Smith J.

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Fig. 6. Reflectance spectra of Vesta extracted from the SINFONI data-cube for three different latitudes of the asteroid. At these wavelengths, the spectrum of Vesta is shaped by the strong absorption band of pyroxene. The spectra have been displayed with a vertical offset to improve clarity. Note the variation of the downward slope of the pyroxene band, which reflects the presence of various types of igneous assemblages on the surface. The Northern hemisphere is dominated by an older eucritic crust (shallower band) while the Southern regions (where a large impact occurred) is dominated by diogenetic assemblage, displaying a deeper pyroxene band.

Et al. 2004, ApJ, 604, L69 Solar System Objects with the NACO Fabry-Perot and SINFONI M. Hartung1 , C. Dumas1 , T. M. Herbst2 , A. Coustenis3 , M. Hirtzig3,4 , ´ amkovics5 , F. Eisenhauer6 , C. deBergh3 and A. Barucci3 M. org Max-Planck-Institut f¨ ur Astronomie, K¨ onigstuhl 17, 69117 Heidelberg, Germany LESIA, Observatoire Paris-Meudon, 92195 Meudon Cedex, France Laboratoire de Plan´etologie et G´eodynamique, 44322 Nantes, France 601 Campbell Hall, Department of Astronomy, University of California, Berkeley, CA 94720, USA Max-Planck-Institut f¨ ur extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany Summary.

E. e. f2 ) with respect to the continuum during the transit. (Note that the small value compared with the error bars is an statistical curiosity. g. 44] · 10−5 ). We also show in this figure the expected change in the index due to a change in f2 as the one detected by STIS–HST (Charbonneau et al. 2002). Therefore, if a signal with an amplitude as the one reported by Charbonneau et al. 44 · 10−5 . ) have performed the experiment only once, and the obtained result is about 2 σ away from the expected value (for a signal as the one detected by Charbonneau et al.

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