P53E-2167
Preliminary Geological Map of the Ac-H-1 Asari Quadrangle of Ceres: An Integrated Mapping Study Using Dawn Spacecraft Data.
Friday, 18 December 2015
Poster Hall (Moscone South)
Lucy-Ann McFadden1, Ottaviano Ruesch1,2, Harald Hiesinger3, Jennifer E. C. Scully4, Thomas Kneissl5, Kynan Hughson6, David A Williams7, Thomas Roatsch8, Frank Preusker8, Nico Schmedemann5, Simone Marchi9, Ralf Jaumann8, Andreas Nathues10, Carol A Raymond4, Christopher T Russell11 and The Dawn Science Team, (1)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (2)GSFC/Oak Ridge Associated Universities, Planetary Systems Laboratory, Greenbelt, MD, United States, (3)University of Münster, Münster, Germany, (4)NASA Jet Propulsion Laboratory, Pasadena, CA, United States, (5)Free University of Berlin, Berlin, Germany, (6)University of California Los Angeles, Los Angeles, CA, United States, (7)Arizona State University, Tempe, AZ, United States, (8)German Aerospace Center DLR Berlin, Berlin, Germany, (9)Southwest Research Institute Boulder, Boulder, CO, United States, (10)Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany, (11)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-1 Asari quadrangle of dwarf planet Ceres. The Dawn Framing Camera observed the quadrangle (north polar area: 66°N-90°N) from an altitude of 4424 km and a clear-filter mosaic was produced at a spatial resolution of 400 m/pixel. A stereo-photogrammetric digital elevation model was calculated from images acquired during a higher altitude resulting in a spatial resolution of 1.4 km/pixel. Key characteristics of the study area are (1) a high density of impact craters and (2) moderate topographic variations. We measured a crater density of 9.8E-04 (km-2) for crater diameters >10 km, the highest on Ceres. Few isolated topographic highs (plateaus), reaching ~5 km in altitude relative to the ellipsoid, are present. Their irregular shape is often sculpted by impacts. We also note a positive relief with relatively steep slopes (~13°) and a cone-like shape centered at 85°N/8°E. Topographic lows, reaching -4 km, correspond to the floors of impact craters with diameters up to 64 km. The morphology of impact craters exhibits varying degrees of degradation. Degraded crater floors show central peaks and mass wasting deposits. The largest morphologically fresh deposit (78°N/38°E) is 20 km long, and has a lobate shape with striations on its surface. It extends from a crater rim downslope. No extensive ejecta deposits are present in the study area. In the course of the ongoing mission, we will incorporate mosaics from the High Altitude Mapping Orbit (~140 m/pixel) and Low Altitude Mapping Orbit (~35 m/pixel) phases to complete the preliminary photo-geological map and stratigraphy.
