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C. Boussin, L. Regalia, J.J. Plateaux, A. Hamdouni (Reims University, France), B.L. Lutz (Northern Arizona Univ.), C. de Bergh (Paris Observatory, France), A. Barbe (Reims University, France)
We have measured broadening and shift coefficients for ro-vibrational lines of the \nu2 and 3\nu2 bands of CH3D, with the most abundant gases in planetary atmospheres (i.e. H2 and He for the giant planets and in the case of Titan, N2) as the foreign buffer gases, using a multispectral fitting technique developed by the Reims group. The spectra of the \nu2 band, near 5 microns, were recorded under high resolution and two temperatures (295 and 197K) using a FTS at the G.S.M.A. Reims laboratory. Those of the 3\nu2 band, near 1.6 microns, were recorded also under high resolution but only at room temperature with the FTS at Kitt Peak National Observatory. Broadening and shift coefficients were determined for lines of \nu2 up to J=20 in the P-branch and up to J=19 in the R-branch. For 3\nu2, measurements were made up to J=14 in the P-branch and up to J=12 in the R-branch. In addition, for \nu2, the temperature dependences of many of these coefficients were derived. Comparisons of the room temperature coefficients for the two bands show strong similarities in both their magnitudes and dependences with J and K. These similarities suggest that the temperature dependence determined for \nu2 can be used for 3\nu2.
The author(s) of this abstract have provided an email address for comments about the abstract: christophe.boussin@univ-reims.fr