Physics
Scientific paper
Jan 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998nvmi.conf...51l&link_type=abstract
Workshop on New Views of the Moon: Integrated Remotely Sensed, Geophysical, and Sample Datasets, p. 51
Physics
Brightness Temperature, Clementine Spacecraft, Infrared Radiation, Lunar Surface, Calibrating, Focal Plane Devices, Imaging Techniques, Mercury Cadmium Tellurides, Lunar Temperature
Scientific paper
The scientific payload on the Clementine spacecraft included a Long-Wave Infrared (LWIR) camera with a single passband of width 1.5 micron centered at a wavelength of 8.75 micron. The LWIR camera had a 128 x 128 mercury cadmium telluride focal plane array and used a catadioptric lens. The field of view of the instrument was 1 degree x 1 degree. The Clementine orbit deviated +/-30 degrees from sun synchronous, and for two lunar months, dayside nadir-looking images were obtained near local noon. The LWIR spatial resolution ranged from 200 m near the poles to 55 m at the equator. Contiguous pole-to-pole imaging strips were obtained with about 10% overlap between adjacent frames. However, significant longitude gaps exist between successive orbital passes. During the systematic mapping phase of the Clementine mission, approximately 220,000 thermal-infrared images of the lunar surface were obtained. Observed LWIR radiances can be converted to brightness temperatures that provide information on various physical properties of the lunar surface. Topography, albedo, and latitude are dominant factors in determining dayside lunar thermal emission. We have completed the calibration of the LWIR camera using both preflight and in-flight data Preflight calibration was performed at Lawrence Livermore National Laboratory in an effort to measure camera characteristics such as radiometric sensitivity, gain and offset scale factors, temporal/spatial noise, and dark-noise dependence on focal-plane array temperatures. The several steps involved in the calibration routine include: converting measured DN values to radiance values; identifying and eliminating bad pixels; correcting for pixel response variation across the detector array; determining the zero-flux background of the instrument; comparing LWIR measured radiances of the Apollo 17 landing site to in situ temperature measurements in order to derive absolute calibration adjustments; and finally, converting measured radiance values to temperatures via the Planck function.
Jakosky Bruce M.
Lawson Stefanie
Mellon Michael T.
Park Seong-Hong
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