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Cassini VIMS observations of the Galilean satellites including the VIMS calibration procedure |
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| Authors: | TB McCord A Coradini F Capaccioni G Filacchione P Cerroni KH Baines J-P Bibring E Bussoletti DP Cruikshank V Formisano Y Langevin RM Nelson B Sicardy |
| Institution: | a HIGP/SOEST, University of Hawaii, POST 502, Honolulu, HI 96822, USA b Planetary Science Institute, 22 Fiddler's Rd., Winthrop, WA 98862-0667, USA c Istituto Fisica Spazio Interplanetario, CNR, Via Fosso del Cavaliere, Roma 00133, Italy d USGS, Mail Stop 964, Box 25046, Denver Federal Center, Denver, CO, USA e Department Pl. Sci. and LPL, University of Arizona, Tucson, AZ 85721-0092, USA f Jet Propulsion Laboratory, Pasadena, CA 91109, USA g Université de Paris Sud-Orsay, IAS, 91405 Orsay Cedex, France h INAF Osservatorio Astronomico di Capodimonte, Napoli, Italy i Departement de Recherche Spatial, 5, Place Jules Jannsen, 92195 Meudon Principal Cedex, France j NASA Ames Research Center, Astrophysics Branch, Moffett Field, CA 94035-1000, USA k Observatoire de Paris-Meudon, 5, Place Jules Jannsen, 92195 Meudon Cedex, France l DLR, Institute for Planet. Expl., Rutherfordstrasse 2, D-12489 Berlin, Germany m Cornell University, 418 Space Science Bldg., Ithaca, NY 14853, USA n University of Nantes, B.P. 92208, 2, rue de la Houssinière, 44072 Nantes Cedex 3, France o Istituto Astrofisica Spaziale e Fisica Cosmica, CNR, Via Fosso del Cavaliere, Roma 00133, Italy |
| Abstract: | The Visual and Infrared Mapping Spectrometer (VIMS) observed the Galilean satellites during the Cassini spacecraft's 2000/2001 flyby of Jupiter, providing compositional and thermal information about their surfaces. The Cassini spacecraft approached the jovian system no closer than about 126 Jupiter radii, about 9 million kilometers, at a phase angle of <90°, resulting in only sub-pixel observations by VIMS of the Galilean satellites. Nevertheless, most of the spectral features discovered by the Near Infrared Mapping Spectrometer (NIMS) aboard the Galileo spacecraft during more than four years of observations have been identified in the VIMS data analyzed so far, including a possible 13C absorption. In addition, VIMS made observations in the visible part of the spectrum and at several new phase angles for all the Galilean satellites and the calculated phase functions are presented. In the process of analyzing these data, the VIMS radiometric and spectral calibrations were better determined in preparation for entry into the Saturn system. Treatment of these data is presented as an example of the VIMS data reduction, calibration and analysis process and a detailed explanation is given of the calibration process applied to the Jupiter data. |
| Keywords: | Satellites Galilean satellites Jupiter system Satellite surfaces Surface composition Space mission |
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