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The Surface of Titan from Adaptive Optics Observations

Published online by Cambridge University Press:  30 March 2016

Seran G. Gibbard ,
Bruce A. Macintosh ,
Claire E. Max ,
Henry Roe ,
Imke de Pater ,
E.F. Young  and
Christopher P. McKay
Seran G. Gibbard
Affiliation:
Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
Bruce A. Macintosh
Affiliation:
Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
Claire E. Max
Affiliation:
Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
Henry Roe
Affiliation:
University of California, Berkeley, CA 94720-3411, USA
Imke de Pater
Affiliation:
University of California, Berkeley, CA 94720-3411, USA
E.F. Young
Affiliation:
Southwest Research Institute, San Antonio, TX 78228-0510, USA
Christopher P. McKay
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035, USA

Abstract

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Saturn’s largest moon Titan is the only satellite in the Solar System with a substantial atmosphere. Photolysis of methane creates a hydrocarbon haze in Titan’s atmosphere that is opaque to visible light. The new adaptive optics system on the 10–meter W. M. Keck Telescope enables us to observe Titan with a resolution of 0.04 arcseconds, or 20 resolution elements across the disk. By observing at near-infrared wavelengths that are methane band windows we can see through Titan’s hydrocarbon haze to the surface beneath. Recent adaptive optics images of Titan both in broadband (J, H, and K) filters and in narrowband filters that selectively probe Titan’s surface and atmosphere allow us to determine surface albedo and properties of the hydrocarbon haze layer. Future observations will include high-resolution spectroscopy coupled with adaptive optics to obtain spectra of individual surface features.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 12: Highlights of Astronomy. As presented at the XXIVth General Assembly of the IAU, 2000 , 2002 , pp. 629
Copyright
Copyright © Astronomical Society of Pacific 2002