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W.C. Maguire, J.C. Pearl, M.D. Smith, R.F. Thompson (NASA/GSFC), B.J. Conrath (Cornell), S. Dason (HSTX), M.S. Kaelberer (RSTX), P.R. Christensen (Arizona State)
Part of the task of interpreting IR spectral features observed by MGS/TES due to surface minerals requires distinguishing those IR signatures from atmospheric signatures of gas and dust.1 Surface-atmosphere separation for MGS/TES depends on knowledge of the retrieved temperature profile. In turn, the temperature retrieval from the observed data depends on molecular parameters including 15 \micron CO2 line shape or line intensities which contribute to defining the Mars synthetic radiative transfer model. Using a simple isothermal, homogeneous single layer model of Pinnock and Shine,2 we find the ratio of (the error in degrees Kelvin of the retrieved temperature profile) to (the percentage error in the absorption coefficient) (deg K/percent) to be 0.4 at 200K. This ratio at 150K and 250K is 0.2 and 0.6, respectively. A more refined model, incorporating observed MGS/TES retrieved temperature profiles, the TES instrumental resolution and the most recent molecular modelling, will yield an improved knowledge of this error sensitivity. We present results of such a sensitivity study to determine the dependence of temperature profiles inverted from MGS/TES on these and other molecular parameters. This work was supported in part by NASA's Mars Data Analysis Program.
1B.J. Conrath, J.C. Pearl, M.D. Smith, W.C. Maguire, S. Dason, M.S. Kaelberer and P.R. Christensen, submitted to JGR, 1999.
2S. Pinnock and K.P. Shine, J. Atmos. Sci. 55 (1998) 1950-1964.