Mars ultraviolet imaging spectrometer experiment on the PLANET-B mission |
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| Institution: | 1. CNRS LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales, Université Versailles St Quentin en Yvelines, Quartier des Garennes, 11 bd d''Alembert, 78280 Guyancourt, France;2. Space Research Institute, 84/32 Profsoyuznaya St, Moscow, Russia;3. CNRS LATMOS, Université Pierre et Marie Curie, 4 place Jussieu, 75252 Paris, France;4. CEA-Saclay, route Nationale, Gif-sur-Yvette, France;5. BIRA-IASB, avenue Circulaire 3, Brussels, Belgium;6. LPAP, Université de Liège, Quartier Agora, 19c allée du 6 août, Liège, Belgium;7. CNRS LMD, 4 place Jussieu, 75252 Paris Cédex, France;8. ESA-ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, Netherland;9. LPL, University of Arizona, Tucson, AZ, United States;10. Institut d''Astrophysique Spatiale, Orsay, France;11. LASP, Boulder, CO, United States;1. Darien High School, Darien, CT 06820, United States of America;2. NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States of America |
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| Abstract: | An ultraviolet imaging spectrometer (UVS) has been developed for the PLANET-B spacecraft. The UVS instrument is composed of a grating spectrometer (UVS-G) and a D/H absorption cell photometer (UVS-P). The UVS-G is a flat-field type spectrometer measuring optical emissions in the FUV and MUV range between 115 nm and 310 nm with a spectral resolution of 2 – 3 nm. The UVS-P is a photometer detecting hydrogen (H) and deuterium (D) Lyman α emissions separately by an absorption cell technique. Scientific targets of the UVS experiment are the investigation of (1) hydrogen and oxygen coronas around Mars, (2) the D/H ratio in the upper atmosphere, (3) dayglow, (4) aurora and nightglow, (5) dust, clouds and ozone, and (6) the surface composition of Phobos and Deimos. |
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