Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21a1647o&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P21A-1647
Physics
[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [5405] Planetary Sciences: Solid Surface Planets / Atmospheres, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
The Mars Atmospheric Trace Molecule Occultation Spectrometer (MATMOS) mission will deploy a high-resolution infrared Fourier transform spectrometer (FTS) to Mars on-board the ExoMars Trace Gas Orbiter in 2016. MATMOS is a joint investigation between the California Institute of Technology, NASA's Jet Propulsion Laboratory, and the Canadian Space Agency (CSA). The instrument will be similar to, and derives a strong heritage from, the CSA's Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) on-board SCISAT. Both MATMOS and ACE-FTS measure the absorption spectra of the atmosphere during solar occultation, making up to 30 measurements per day, one at each satellite sunrise and sunset.ACE-FTS analyzes CO2 to determine temperature and pressure as functions of altitude, then simultaneously retrieves vertical profiles of volume mixing ratio (VMR) for more than two dozen gases using least squares minimization. MATMOS will make use of the GGG analysis suite developed for the MkIV balloon flights, the Atmospheric Trace Molecule Spectroscopy experiment and the ground-based Total Carbon Column Observatory Network. Both retrieval methods divide the spectra into smaller spectral windows and use a Voigt instrument line shape. Their forward models are similar and divide the atmosphere into layers that are assumed to have constant temperature, pressure, and VMR for each molecule. GGG uses the inverse method and its own nonlinear least-squares fitting program to derive partial columns along the optical slant path and to retrieve VMR profiles. MATMOS will inventory the composition of the Martian atmosphere with a sensitivity 2-3 orders of magnitude better than any previous instrument. In order to prepare the GGG analysis suite for the upcoming MATMOS mission, 25 ACE occultations have been analyzed using GGG and compared to the ACE-FTS v3.0 retrievals. This work examines the differences between the two algorithms, identifies those that produce inconsistencies between retrieved VMR profiles, and presents the results of adapting the GGG software and input data to minimize those inconsistencies. The results obtained using the ACE-FTS spectral windows are compared with those obtained using MkIV balloon windows. Adjustments to the algorithm's assumptions, such as modifying the forward model, instrument line shape, and apodization, are evaluated. The geometry used to determine tangent locations and heights is optimized. Synthetic spectra for the Martian atmosphere are calculated using GGG, data from the Mars Climate Database, and known upper limits for MATMOS target gases. VMR profiles are retrieved from the spectra with GGG and evaluated. The study is generalized to several locations at polar and tropical latitudes and will culminate with the inclusion of dust in the synthetic spectra.
Boone Carl
Olsen K. S.
Strong Keith
Toon Geoffrey C.
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