Planets

A new 1.6-micron map of Titan's surface

  1. H. G. Roe1,
  2. I. de Pater2,
  3. S. G. Gibbard3,
  4. B. A. Macintosh3,
  5. C. E. Max4,
  6. E. F. Young5,
  7. M. E. Brown1,
  8. A. H. Bouchez6

Article first published online: 17 JUN 2004

DOI: 10.1029/2004GL019871

Issue

Geophysical Research Letters

Geophysical Research Letters

Volume 31, Issue 17, September 2004

Additional Information

How to Cite

Roe, H. G., I. de Pater, S. G. Gibbard, B. A. Macintosh, C. E. Max, E. F. Young, M. E. Brown, and A. H. Bouchez (2004), A new 1.6-micron map of Titan's surface, Geophys. Res. Lett., 31, L17S03, doi:10.1029/2004GL019871.

Author Information

  1. 1

    Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA

  2. 2

    Department of Astronomy, University of California, Berkeley, California, USA

  3. 3

    Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, California, USA

  4. 4

    Center for Adaptive Optics, University of California, Santa Cruz, California, USA

  5. 5

    Southwest Research Institute, Boulder, Colorado, USA

  6. 6

    W. M. Keck Observatory, Waimea, Hawaii, USA

Publication History

  1. Issue published online: 17 JUN 2004
  2. Article first published online: 17 JUN 2004
  3. Manuscript Accepted: 19 APR 2004
  4. Manuscript Revised: 13 APR 2004
  5. Manuscript Received: 2 MAR 2004

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[1] We present a new map of Titan's surface obtained in the spectral ‘window’ at ∼1.6 μm between strong methane absorption. This pre-Cassini view of Titan's surface was created from images obtained using adaptive optics on the W.M. Keck II telescope and is the highest resolution map yet made of Titan's surface. Numerous surface features down to the limits of the spatial resolution (∼200–300 km) are apparent. No features are easily identifiable in terms of their geologic origin, although several are likely craters.

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