Other
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p52a0369b&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P52A-0369
Other
5410 Composition, 5464 Remote Sensing, 5470 Surface Materials And Properties, 6225 Mars
Scientific paper
Imaging spectroscopy of Mars from 2.19 to 4.12 μm at high spectral resolution (λ /Δλ 800-2300) were collected in April 1999 using the cryogenic long slit spectrometer at the KPNO 2.2 m telescope. These data have been used to model the cloud optical depth, particle sizes, and ice aerosol content of the aphelion cloud belt and to monitor diurnal changes in clouds (Glenar et al. 2002, in press Icarus). The detailed modeling of cloud properties permits us to now identify regions where the atmosphere is clear and to look for variations in the 3 μm bound water band on the Martian surface. Observations of the same locations of the planet under different viewing geometries (and local times of day) permit independent verification of shape of the surface feature and quantify viewing angle effects. The high spectral resolution also enables the identification of atmospheric features, solar lines, residual telluric absorptions, and weak surface features. Initial analysis has focused on regions north of 30° N latitude (outside the aphelion cloud belt) between ~150° and 300° West, and away from orographic clouds. TES has identified two crustal units: Type I (basaltic) and Type II (basaltic andesite) (Banfield et al. 2000). Recently, an alternative interpretation has been suggested for the Type II unit as a weakly altered basalt (Wyatt and McSween 2002). One region in our data set (~30°-50° N latitude and ~260°-280° W longitude) was mapped as Type II. Careful comparison of the Type II material to the Type I basaltic unit and the Martian bright regions should permit an assessment of the relative hydration state of the Type II materials and help resolve this debate. The attempt to identify Type I regions that are cloud free in our data set is underway but may be problematic due to its association with volcanos (which develop orographic clouds) and to its equatorial distribution affected by the aphelion cloud belt. Additionally, other effects such as grain size, cementation, and viewing geometry need to be accessed before directly comparing band depths. No evidence for carbonates has been found.
Bjoraker Gordon L.
Blaney Diana L.
Glenar David A.
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