Regional and Local Temperature Maps of Dwarf Planet Ceres from Dawn/VIR

Friday, 18 December 2015
Poster Hall (Moscone South)
Federico Tosi1, Francesca Zambon1, Maria Teresa Capria1, Filippo Giacomo Carrorro1, Mauro Ciarniello1, Maria Cristina De Sanctis1, Andrea Longobardo1, Andrea Raponi1, Eleonora Ammannito2, Jean Philippe Combe3, Harald Hiesinger4, Jian-Yang Li5, Lucy A McFadden6, Norbert Schorghofer7, Stefan Schroeder8, Katrin Stephan9, Marc Rayman10, Carol A Raymond10 and C. T. Russell2, (1)IAPS-INAF, Rome, Italy, (2)University of California Los Angeles, Los Angeles, CA, United States, (3)Bear Fight Institute, Winthrop, WA, United States, (4)University of Münster, Münster, Germany, (5)Planetary Science Institute Tucson, Tucson, AZ, United States, (6)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (7)Univ of Hawaii at Manoa, Honolulu, HI, United States, (8)German Aerospace Center DLR Berlin, Berlin, Germany, (9)German Aerospace Center, Berlin, Germany, (10)NASA Jet Propulsion Laboratory, Pasadena, CA, United States
Since the beginning of 2015, the Visible InfraRed (VIR) mapping spectrometer onboard the NASA Dawn mission has obtained hyperspectral images of Ceres, with improving spatial resolution. VIR operates in the overall spectral range 0.25-5.1 µm, with the main goal of inferring the surface composition of the target in its uppermost layer, as thick as tens of microns.

Taking advantage of the wavelength range longward of 3 µm, VIR can be used as a thermal mapper, i.e. as a tool to derive thermal images and spatially-resolved temperature maps. To do this, the VIR team uses a Bayesian approach to nonlinear inversion that was extensively applied to the Vesta dataset earlier.

Already in February 2015, VIR had the chance to acquire data with a spatial resolution of ~11 km/px. Those temperature images revealed that a spot of high-albedo (bright) material, highlighted by the Hubble Space Telescope (HST) earlier and recently associated with the crater Haulani, was cooler than sorrounding regions seen under similar solar illumination, whereas the brightest spots on Ceres, in the crater Occator, did not display any thermal contrast. The following Survey phase yielded hyperspectral coverage of Ceres at ~1.3 km/px, and the High Altitude Mapping Orbit (HAMO) phase starting in mid-August 2015 is expected to provide VIR data with a resolution of ~0.4 km/px. These datasets allow derivation of regional and local temperature maps as well as the study of thermal anomalies at those spatial scales. Due to the low overall thermal inertia of Ceres, the surface temperature is essentially dominated by the instantaneous value of the solar incidence angle. Small values of this angle result in high surface temperatures, and, unlike Vesta, the low obliquity of Ceres (~4°) does not result in observable seasonal effects for a given location on the surface. However, different responses to insolation as observed at the local scale may be indicative of differences in density/porosity and thermal conductivity, which is key to constrain thermo-physical modeling.