THE CASSINI ULTRAVIOLET IMAGING SPECTROGRAPH INVESTIGATION 1, 1 1 LARRY W. ESPOSITO ∗, CHARLES A. BARTH , JOSHUA E. COLWELL , GEORGE M. LAWRENCE1, WILLIAM E. McCLINTOCK1,A. IAN F. STEWART1, H. UWE KELLER2, AXEL KORTH2, HANS LAUCHE2, MICHEL C. FESTOU3,ARTHUR L. LANE4, CANDICE J. HANSEN4, JUSTIN N. MAKI4,ROBERT A. WEST4, HERBERT JAHN5, RALF REULKE5, KERSTIN WARLICH5, DONALD E. SHEMANSKY6 and YUK L. YUNG7 1University of Colorado, Laboratory for Atmospheric and Space Physics, 1234 Innovation Drive, Boulder, CO 80303, U.S.A. 2Max-Planck-Institut fur¨ Aeronomie, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany 3Observatoire Midi-Pyren´ ees,´ 14 avenue E. Belin, F31400 Toulouse, France 4JetPropulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, U.S.A. 5Deutsches Zentrum fur¨ Luft und Raumfahrt, Institut fur¨ Weltraumsensorik und Planetenerkundung, Rutherford Strasse 2, 12489 Berlin, Germany 6University of Southern California, Department of Aerospace Engineering, 854 W. 36th Place, Los Angeles, CA 90089, U.S.A. 7California Institute of Technology, Division of Geological and Planetary Sciences, MS 150-21, Pasadena, CA 91125, U.S.A. (∗Author for correspondence: E-mail:
[email protected]) (Received 8 July 1999; Accepted in final form 18 October 2000) Abstract. The Cassini Ultraviolet Imaging Spectrograph (UVIS) is part of the remote sensing payload of the Cassini orbiter spacecraft. UVIS has two spectrographic channels that provide images and spectra covering the ranges from 56 to 118 nm and 110 to 190 nm. A third optical path with a solar blind CsI photocathode is used for high signal-to-noise-ratio stellar occultations by rings and atmospheres. A separate Hydrogen Deuterium Absorption Cell measures the relative abundance of deuterium and hydrogen from their Lyman-α emission.