Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusm.p32a..03k&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #P32A-03
Physics
5405 Atmospheres: Composition And Chemistry, 5409 Atmospheres: Structure And Dynamics, 5464 Remote Sensing, 6225 Mars
Scientific paper
Observations of the CO (2-0) band at 2.35 μ m from the Phobos orbiter were interpreted in favor of high variability of the CO mixing ratio in the Martian atmosphere. Theory does not support this effect, and ground-based high-resolution spectroscopy in the infrared and microwave regions showed that the variations does not exceed a factor of 2. However, the smallest locations studied were of 0.4 Mars' radius, that is, much larger than those observed with the Phobos. I observed Mars on April 20 2001 using the cryogenic echelle long-slit spectrograph (CSHELL) at NASA IRTF. The chosen spectral range covered four lines (P6-P9) of the CO (3-0) band at 1.58 μ m. Two-way optical depths of CO in the line centers are close to one and therefore the best for measurements. The instrument resolving power was 40,000. Changing a slit position on the Martian disk with an increment of 0.5 arc sec, the full Mars disk was mapped. The observing conditions were excellent and provided a point spread fuction of 0.5 arc sec, that is, 0.08 Mars' radius and significantly better than in the previous ground-based studies of the CO variations. The observed spectra include many CO2 lines. Some of these lines are comparable in equivalent widths to the CO lines and may be used to obtain the CO mixing ratio and study its variations. Data processing, analysis, the obtained results and their interpretation are discussed.
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