The 5-to-7 micron Spectrum of Titan Measured with ISO/SWS

Details The 5-to-7 micron Spectrum of Titan Measured with ISO/SWS The 5-to-7 micron Spectrum of Titan Measured with ISO/SWS

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998dps....30.3902c&link_type=abstract

American Astronomical Society, DPS meeting #30, #39.02; Bulletin of the American Astronomical Society, Vol. 30, p.1087

Astronomy and Astrophysics

Astronomy

Scientific paper

In January 1997, ISO observed Titan between 1430 and 1900 cm(-1) (lambda =5.3--7 micron) using one of the grating modes of the SWS spectrometer. Although, the nominal spectral resolution was twice as good, the calibrated data were binned in 3 cm(-1) intervals in order to achieve sufficient signal-to-noise. Globally, the flux density decreases rapidly from a maximum of about 2.5 Jy at 1430--1480 cm(-1) to 0.1 Jy near 1800 cm(-1) . In addition, there is a narrow and prominent emission feature near 1540 cm(-1) . This part of Titan's spectrum has already been explored by the IRIS instrument on Voyager 1 with a comparable resolution but only up to 1580 cm(-1) . The two data sets compare very nicely. We interpret this spectrum with a radiative transfer model including the following components: a) a thermal continuum due to the photochemical haze, b) stratospheric emission due to the nu_ {4} and nu_ {2} bands of CH4, and to the nu_ {8} band of C2H6, c) sunlight backscattered by the haze and the surface. Thermal emission dominates up to 1700 cm(-1) . Reflected sunlight picks up at 1650 cm(-1) and becomes dominant above 1800 cm(-1) . A good match is obtained with the following model parameters: a stratospheric CH4 mole fraction of about 2%; a C2H6 mole fraction of 7x 10(-6) around 100 km (and moderately increasing with altitude); an imaginary index of refraction for the haze 1--3 times larger than that of N2-CH4 tholins; and a surface albedo of about 0.10.

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