Mapping Water Ice Clouds and Ozone on Mars with MRO/MARCI

Details Mapping Water Ice Clouds and Ozone on Mars with MRO/MARCI Mapping Water Ice Clouds and Ozone on Mars with MRO/MARCI

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.3004w&link_type=abstract

American Astronomical Society, DPS meeting #42, #30.04; Bulletin of the American Astronomical Society, Vol. 42, p.1028

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The Mars Color Imager (MARCI) instrument (aboard the Mars Reconnaissance Orbiter, MRO) is a``push-frame,'' wide-angle imager whose overall components, capabilities, and performance (including calibration methodology) are described in recent publications (e.g., Malin et al., 2008, Icarus; Bell et al., 2010, Icarus). Of particular note for atmospheric studies is the presence of two ultraviolet (UV) bands (centered near 265 and 330 nm) which allow for the direct retrieval of column-integrated water ice cloud optical depths and ozone abundances. MARCI observations in the UV provide global daily mapping of these two atmospheric constituents. For computationally efficiency, the retrievals employ the "look-up table" approach, where each of the relevant input parameters (photometric angles, aerosol optical depths, ozone abundance) is tessellated over the sampled or expected range of values (table generation employs the DISORT package developed by K. Stamnes and collaborators). The UV aerosol properties are taken from the recent analyses of the MARCI 2007 global dust event observations (Wolff et al., 2010, Icarus) and the empirical extension of the TES solarband water ice properties (e.g., Clancy et al., 2003, JGR). Empricial studies indicate that a precision of 0.05 on cloud optical depths and 1-2 micron-atm for ozone. In our presentation, we will focus on a synopsis of the general seasonal behavior observed during the first MRO mapping year.
This work was supported by NASA through JPL Contract 1275776

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