Computer Science – Databases
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusm.p41c..03k&link_type=abstract
American Geophysical Union, Spring Meeting 2007, abstract #P41C-03
Computer Science
Databases
0343 Planetary Atmospheres (5210, 5405, 5704), 5405 Atmospheres (0343, 1060), 5410 Composition (1060, 3672), 5455 Origin And Evolution, 6225 Mars
Scientific paper
The major problems in spectroscopic determinations of the oxygen and carbon isotope ratios on Mars are uncertainties associated with (1) equivalent widths of the observed absorption lines, (2) line strengths in spectroscopic databases, and (3) thermal structure of the Martian atmosphere during the observation. We have made special efforts to reduce all these uncertainties. We observed Mars using Fourier Transform Spectrometer at the Canada-France-Hawaii Telescope. While the previous measurements of the oxygen and carbon isotope ratios on Mars were byproducts in observations of other species, our observation was specifically aimed at the isotope ratios. The observation covered a range of 6020 to 6310 cm-1 with the highest resolving power of 400,000 and a signal-to-noise ratio of 180 in the middle of the spectrum. The chosen spectral range involves 512 lines of the main isotope, 197 lines of 13CO2, 184 lines of CO18O, and 120 lines of CO17O. (Lines with strengths exceeding 10-27 cm at 220 K are considered here.) Due to the high spectral resolution, most of the lines are not blended. Uncertainties of retrieved isotope abundances are in inverse proportion to resolving power, signal-to-noise ratio, and square root of the number of lines. One of us (R.A. Toth) is making laboratory studies of the CO2isotope line strengths in the range of our observation. This work is aimed to achieve an accuracy of ~1% in the line strengths. Detailed observations of temperature profiles and dust abundances using MGS/TES are used to simulate each absorption line at various heights in each part of the instrument field of view and then sum up the results. Thermal radiation of Mars' surface and atmosphere is negligible in the chosen spectral range, and this reduces errors associated with uncertainties in the thermal structure on Mars. Using a combination of all these factors, we plan to achieve the highest accuracy in measuring the CO2isotope ratios. The results will be reported.
Krasnopolsky Vladimir A.
Maillard Jacques
Owen Tobias C.
Smith Masson D.
Toth Robert A.
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