HCl, HF, CO and CO2 analysis in the upper atmosphere of Venus from SOIR spectra

Details HCl, HF, CO and CO2 analysis in the upper atmosphere of Venus from SOIR spectra HCl, HF, CO and CO2 analysis in the upper atmosphere of Venus from SOIR spectra

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..228w&link_type=abstract

European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a

Physics

Optics

Scientific paper

The SOIR spectrometer is a new Solar Occultation IR spectrometer operating in the 2.2-4.3 μm range at a resolution of 0.12 cm-1, the highest onboard Venus Express. This new concept combines an echelle grating and an Acousto Optical Tunable Filter (AOTF) to sort out one diffraction order at a time. The wavelength window probed by SOIR allows a detailed chemical inventory of the Venus atmosphere above the cloud layer (65 to 150 km) with an emphasis on the vertical distribution of the gases. Recent advances in the characterization of the instrument and in particular of the band pass response of the AOTF [1] lead to a better comprehension of the diffraction order overlapping, which is crucial for the accurate retrieval of SOIR spectra using ASIMUT [2]. This allowed us to routinely perform measurements of HCl, HF and CO vertical profiles and to investigate the geographical, temporal and solar time dependency of these concentration profiles. As the instrument is able to record spectra from 4 different orders during the same solar occultation, CO2, the major constituent of the Venus atmosphere, was also measured, allowing vmr determination of the minor gases. Our results are compared to the Venus International Reference Atmosphere (VIRA model, [3]) and to measurements of previous missions. It was shown recently that the instrument is able to detect various isotopologues of the CO2 [4] and of the H2O [5] molecules. In addition we now show spectra exhibiting absorption lines from H35Cl and H37Cl transitions. Simultaneous measurements of these isotopologues can be used to determine atomic isotopic ratios on Venus for comparison with those on Earth, as both planets have a common origin. References [1] Mahieux, A., et al. (2008) Applied Optics, 47(13), 2252-2265. [2] Vandaele, A.C., et al. (2008) JGR (accepted for publication). [3] Zasova, L., et al. (2006) Cosmic Res., 44(4), 364- 383. [4] Wilquet, V., et al. (2008) JQSRT, 109, 895-905. [5] Fedorova, A., et al. (2008) JGR (submitted).

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