Probing Titan's lower atmosphere with acousto-optic tuning

Details Probing Titan's lower atmosphere with acousto-optic tuning Probing Titan's lower atmosphere with acousto-optic tuning

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icar..163..150c&link_type=abstract

Icarus, Volume 163, Issue 1, p. 150-163.

Physics

Optics

16

Scientific paper

Narrow-band images of Titan were obtained in November 1999 with the NASA/GSFC- built acousto-optic imaging spectrometer (AImS) camera. This instrument utilizes a tunable filter element that was used within the 500- to 1050-nm range, coupled to a CCD camera system. The images were taken with the Mount Wilson 2.54-m (100 in.) Hooker telescope, which is equipped with a natural guide star adaptive optics system. We observed Titan at 830 and 890 nm and at a series of wavelengths across the 940-nm window in Titan's atmosphere where the methane opacity is relatively low. We determined the absolute reflectivity (I/F) of Titan and fit the values at 940 nm to a Minnaert function at Titan's equator and at -30° latitude (closer to the subsolar point) and obtained average values for the Minnaert limb-darkening slope, k, of 0.661 +/- 0.007 and 0.775 +/- 0.018, respectively. Comparison with models suggests that the equatorial value of k is consistent with rain removal of haze in the lower atmosphere. The higher value of k at -30° is consistent with the southern hemisphere being brighter than the equator. However, the fits are not unique. The data and models at 890 are consistent with no limb brightening or darkening at this wavelength either at the equator or at -30°.

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