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Determining Titan's Spin State from Cassini RADAR Images

  • Authors: Bryan W. Stiles, Randolph L. Kirk, Ralph D. Lorenz, Scott Hensley, Ella Lee, Steven J. Ostro, Michael D. Allison, Philip S. Callahan, Yonggyu Gim, Luciano Iess, Paolo Perci del Marmo, Gary Hamilton, William T. K. Johnson, Richard D. West, and the Cassini RADAR Team

STILES et al. 2008 The Astronomical Journal 135 1669.

  • Provider: AAS Journals

Caption: Figure 1.

Example of a landmark: the panel on the left is from Titan flyby T25. The panel on the right is from flyby T28. An arrow indicates the landmark. The vertical line on the left is 10 km long. Using the zero-obliquity IAU Titan spin model, landmarks could be misplaced between images by more than 30 km. Using the spin model reported here, the misplacement distances are reduced to 1–2 km. The figure depicts a 3.5 km vertical shift in landmark location between panels in order to illustrate the ease with which the human eye can detect km scale misregistration.

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