Paper No. 308-12
Presentation Time: 9:00 AM-6:30 PM
INITIAL GEOLOGICAL MAPPING OF THE AC-H-12 TOHARU QUADRANGLE OF CERES USING DAWN SPACECRAFT DATA
MEST, Scott C.1, WILLIAMS, David A.
2, CROWN, David A.
1, YINGST, R. Aileen
3, SCHENK, Paul M.
4, JAUMANN, Ralf
5, ROATSCH, Thomas
6, NATHUES, Andreas
7, RUSSELL, Christopher T.
8 and RAYMOND, Carol A.
9, (1)Planetary Science Institute, Tucson, AZ 85719, (2)School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287, (3)Planetary Science Institute, 1700 E. Fort Lowell Rd., Suite 106, Tucson, AZ 85719, (4)Lunar and Planetary Institute, Universities Space Research Association, 3600 Bay Area Boulevard, Houston, TX 77058, (5)Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, Berlin, 12489, Germany, (6)German Aerospace Center (DLR), Institute of Planetary Research, Rutherfordstr. 2, Berlin, 12489, Germany, (7)Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, Goettingen, 37077, Germany, (8)Earth and Space Sciences, University of California, Los Angeles, 595 Charles Young Drive East, Box 951567, Los Angeles, CA 90095-1567, (9)Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, mest@psi.edu
We are using recent data from the Dawn spacecraft to map the geology of the Ac-H-12 Toharu Quadrangle (21-66°S, 90-180°E) of the dwarf planet Ceres in order to examine its surface geology and understand its geologic history. At the time of this writing, mapping was performed on Framing Camera (FC) mosaics from late Approach (1.3 km/px) and Survey (415 m/px) orbits, including clear filter and color images and digital terrain models derived from stereo images. Images from the High Altitude Mapping Orbit (140 m/px) will be used to refine the map in Fall 2015, followed by the Low Altitude Mapping Orbit (35 m/px) starting in December 2015.
The quad is named after crater Toharu (87 km diameter; 49°S, 155°E). The southern rim of Kerwan basin (284 km diameter) is visible along the northern edge of the quad, which is preserved as a low-relief scarp. This quad exhibits smooth terrain in the north, and more heavily cratered terrain in the south. The smooth terrain forms nearly flat-lying plains in some areas, such as on the floor and to the southeast of Kerwan, and overlies hummocky materials in other areas. These smooth materials extend over a much broader area to the north and west than what is represented in this quad, and appear to contain some of the lowest crater densities on Ceres’ surface. Impact craters throughout the quad exhibit a range of coinciding sizes and preservation styles. Smaller craters (<40 km) generally appear morphologically “fresh”, and their rims are nearly circular and raised above the surrounding terrain, although some smaller craters display hexagonal forms. Larger craters, such as Toharu, appear more degraded, exhibiting irregularly shaped rim structures with scalloping along their walls and debris lobes on their floors, indicating collapse of material. Many craters in the area (>20 km) contain central mounds; at current FC resolution, it is difficult to discern if these are primary structures (i.e., central peaks) or secondary features.
Support by D.L. Buczkowski, J.E.C. Scully, C.M. Pieters, F. Preusker, M. Hoffmann, M. Schaefer, S. Marchi, M.C. De Sanctis, and the Dawn Instrument, Operations, and Science Teams is gratefully acknowledged. This work is supported by grants from NASA through the Dawn project, and from the German Space Agency.
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