P53E-2177
Preliminary Geological Maps of the Ac-H-10 Rongo and Ac-H-15 Zadeni Quadrangles: An integrated Mapping Study Using Dawn Spacecraft Data

Friday, 18 December 2015
Poster Hall (Moscone South)
Thomas Platz1, Andreas Nathues1, David A Crown2, Scott C Mest3, David A Williams4, Martin Hoffmann1, Michael Schäfer1, Hanna G Sizemore2, R Aileen Yingst3, Ottaviano Ruesch5, Debra Buczkowski6, Thomas Kneissl7, Nico Schmedemann7, Kynan Hughson8, Frank Preusker9 and Christopher T Russell10, (1)Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany, (2)Planetary Science Institute Tucson, Tucson, AZ, United States, (3)Planetary Science Institute, Tucson, AZ, United States, (4)Arizona State University, Tempe, AZ, United States, (5)GSFC/Oak Ridge Associated Universities, Planetary Systems Laboratory, Greenbelt, MD, United States, (6)JHU Applied Physics Laboratory, Laurel, MD, United States, (7)Free University of Berlin, Berlin, Germany, (8)University of California Los Angeles, Los Angeles, CA, United States, (9)German Aerospace Center (DLR), Berlin, Germany, (10)University of California Los Angeles, IGPP/EPSS, Los Angeles, CA, United States
Abstract:
We used geologic mapping applied to Dawn spacecraft data as a tool to understand the geologic history of the Ac-H-10 Rongo and Ac-H-15 Zadeni quadrangles of dwarf planet Ceres. These regions, Rongo and Zadeni, are located between 22°S-22°N and 288°-360°E and 65-90°S and 0°-360°E, respectively. The Rongo Quadrangle hosts a number of features: 1) the southwest portion is dissected by curvilinear structures likely caused by Yalode basin formation; 2) the central part is marked by dome-like constructs up to 100 km across; 3) a peculiar bright, c.4 km tall, conical structure informally known as the ‘pyramid’; 4) impact craters of various diameters appear moderately to highly degraded or are partially buried; and 5) bright material is primarily exposed in the central portion and often associated with craters. Rongo crater (68 km across) exhibits a central peak and scalloped walls indicative of its degraded appearance. The Zadeni Quadrangle is characterised by impact craters up to 130 km in diameter of which Zadeni crater is the largest. Impact craters across all sizes exhibit fresh to highly degraded morphologies or are partially buried. Many craters developed central peaks. Inter-crater plains are generally hummocky with isolated regions of smooth-textured surfaces. The south pole area (85-90°S) is poorly illuminated and may host a large impact structure. At the time of this writing geologic mapping was performed on Framing Camera (FC) mosaics from Approach (1.3 km/px) and Survey (415 m/px) orbits, including clear filter and colour images and digital terrain models derived from stereo images. In Fall 2015 images from the High Altitude Mapping Orbit (140 m/px) will be used to refine the mapping, followed by Low Altitude Mapping Orbit (35 m/px) starting in December 2015.

Support of the Dawn Instrument, Operations, and Science Teams is acknowledged. This work is supported by grants from NASA through the Dawn project, and from the German and Italian Space Agencies.

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