Near- and mid-Infrared Resolved Imaging of Titan's Atmosphere

Details Near- and mid-Infrared Resolved Imaging of Titan's Atmosphere Near- and mid-Infrared Resolved Imaging of Titan's Atmosphere

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.1703r&link_type=abstract

American Astronomical Society, DPS Meeting #32, #17.03; Bulletin of the American Astronomical Society, Vol. 32, p.1023

Physics

Optics

1

Scientific paper

We present spatially resolved images of Titan in the near-infrared (1-2.5 μ m) with the W.M. Keck Observatory Adaptive Optics (AO) system and in the mid-infrared (8-13 μ m) with the Keck Long Wave Spectometer (LWS). On 30 October 1999 (UT) we observed a bright cloud band at 70° S latitude in two narrowband filters (each ~1% bandwidth centered on 1.158 μ m and 1.702 μ m) chosen such that they selectively probe the atmosphere above the tropopause. The feature was spatially unresolved in latitude and extended over all visible longitudes. From measurements of a star, the AO system achieved a spatial resolution at 1.158 μ m of 0.032'', or 190 km on Titan. Further, we observed a broad haze band extending over approximately 60o of latitude centered slightly south of Titan's equator. This feature is apparent in near-infrared AO images from October 1999. Mid-infrared LWS images from September and November 1999 with a resolution of ~0.2'' show structure across the disk of Titan, and we compare these with models of haze thermal emission in order to determine the haze distribution. HGR is funded by a NASA-GSRP fellowship. This research was supported in part by the STC Program of the National Science Foundation under Agreement No. AST-9876783, and in part under the auspices of the US Department of Energy at Lawrence Livermore National Laboratory, Univ. of Calif. under contract No. W-7405-Eng-48.

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