ISO Spectroscopy of Titan

Details ISO Spectroscopy of Titan ISO Spectroscopy of Titan

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000esasp.456...13c&link_type=abstract

ISO beyond the peaks: The 2nd ISO workshop on analytical spectroscopy. Eds. A. Salama, M.F.Kessler, K. Leech & B. Schulz. ESA-SP

Computer Science

3

Titan, Ir, Spectroscopy, Atmosphere, Surface

Scientific paper

In the spectroscopic mode, Titan was observed by ISO in 1997 by SWS/Grating, PHT-S and CAM/CVF. The combination of these data provides Titan's spectrum from 5 to 17 and from 2.5 to 5 μm with resolving powers ranging from 40 (CAM/CVF) to 2000 (SWS). The analysis of the spectra provides information on (a) Titan's atmospheric structure (temperature and composition) and (b) Titan's surface (through the emission observed in the 2.9-micron window). In this paper we concentrate on the 7 to 9 and 2.5 to 5 micron regions. A temperature profile for Titan's disk is inferred from the analysis of the 7.7 μm CH4 band. The CH3D abundance is estimated to be 7.5 (+4.0-3.7) × 10-6, for a D/H ratio of 9.5 (+9.5-1.0) × 10-5. The 2.9 methane ``window'' on Titan is observed in its full shape for the first time. It shows two peaks at 2.7 and 2.8 μm, and an absorption feature at 2.75 μm, which may be the spectral signature of a surface component on Titan.

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