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2 June 1995 UV/visible camera for the Clementine mission
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This article describes the Clementine UV/Visible (UV/Vis) multispectral camera, discusses design goals and preliminary estimates of on-orbit performance, and summarized lessons learned in building and using the sensor. While the primary objective of the Clementine Program was to qualify a suite of 6 light-weight, low power imagers for future Department of Defense flights, the mission also has provided the first systematic mapping of the complete lunar surface in the visible and near-IR spectral regions. The 410 g, 4.65 W UV/Vis camera uses a 384 X 288 frame-transfer silicon CCD FPA and operates at 6 user-selectable wavelength bands between 0.4 and 1.1 micrometers . It has yielded lunar imagery and mineralogy data with up to 120 m spatial resolution (band dependent) at 400 km periselene along a 39 km cross-track swath.
© (1995) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Joseph F. Kordas, Isabella T. Lewis, Robert E. Priest, W. Travis White III, Darron P. Nielsen, Hye-Sook Park, Bruce A. Wilson, Michael J. Shannon, Arno G. Ledebuhr, and Lyn D. Pleasance "UV/visible camera for the Clementine mission", Proc. SPIE 2478, Space Telescopes and Instruments, (2 June 1995);


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