Probing Titan’s lower atmosphere with acousto-optic tuning

摘要: Abstract 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 500- to 1050-nm range, coupled CCD camera system. The taken Mount Wilson 2.54-m (100 in.) Hooker telescope, which is equipped natural guide star adaptive optics We observed at 830 and 890 nm series wavelengths across 940-nm window Titan’s atmosphere where methane opacity relatively low. determined absolute reflectivity (I/F) fit values 940 Minnaert function equator −30° latitude (closer subsolar point) average for limb-darkening slope, k, 0.661 ± 0.007 0.775 0.018, respectively. Comparison models suggests equatorial value k consistent rain removal haze lower atmosphere. higher southern hemisphere being brighter than equator. However, fits are not unique. data no limb brightening or darkening this wavelength either −30°.