GSA Annual Meeting in Denver, Colorado, USA - 2016

Paper No. 166-9
Presentation Time: 9:00 AM-6:30 PM


ZAMBON, Francesca1, CARROZZO, Filippo Giacomo1, TOSI, Federico1, CIARNIELLO, Mauro1, COMBE, Jean-Philippe2, DE SANCTIS, Maria Cristina3, AMMANNITO, Eleonora4, LONGOBARDO, Andrea5, RAPONI, Andrea1, PALOMBA, Ernesto1, MCFADDEN, Lucy6, PLATZ, Thomas7, STEPHAN, Katrin8, KROHN, Katrin9, FRIGERI, Alessandro1, RUSSELL, Christopher T.10 and RAYMOND, Carol A.11, (1)INAF - Istituto Nazionale di Astrofisica, IAPS - Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere, 100, Rome, I-00133, Italy, (2)Bear Fight Institute, P.O. Box 667, 22 Fiddler's Rd, Winthrop, WA 98862, (3)INAF, Instituto di Astrofisica e Planetolgia Spaziali, Rome, 00133, Italy, (4)Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, Goettingen, 37077, Germany, (5)IAPS - Istituto di Astrofisica e Planetologia Spaziali, INAF - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, Rome, I-00133, Italy, (6)NASA Goddard Space Flight Center, Greenbelt, MD 20771, (7)Max Planck Institute for Solar System Research, Göttingen, 37077, Germany, (8)German Aerospace Center, Institute of Planetary Research, Rutherfordstrasse 2, Berlin, 12489, Germany, (9)Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, Berlin, 12489, Germany, (10)Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, (11)Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109,

After more than one year orbit around Ceres, Dawn spacecraft covered large part of its surface, allowing for a global mineralogical mapping of the entire surface. For mapping purposes, likewise for Vesta, also Ceres’ surface has been divided in 15 quadrangles. Here we describe the quadrangle Ac-H-10 Rongo located in the equatorial region (288°-360°E, 22S-22N) of Ceres. VIR, the visible and infrared spectrometer onboard Dawn, acquired data at different spatial resolutions, allowing for identify the various mineralogical phases characteristic of Ceres surface, at global and local scale [1,2]. Ceres spectra present several bands in the spectral region between 2.5 and 4-µm. Spectral parameters retrieved by VIR data indicate a widespread distribution of NH4-phillosilicates, and OH-rich clays [1]. Rongo quadrangle contains about five gelogical units [3], not always associated with mineralogical variations. The depth of the 3.1-µm band, due to the presence of NH4–Phyllosicates, is quite homogeneous except for some localized regions in which this band appear shallower, and a similar trend is observed for the OH-singnature at 2.7-µm. The dominant feature of this quadrangle is Ahuna Mons, a unique case on Ceres [4]. Ahuna Mons is the largest mountain of the dwarf planet, and conversely to other geological units, shows a spectral parmeters variation with respect to other areas, linked to mineralogical differences.

[1] De Sanctis et al., 2015 Nature

[2] Ammannito et al., 2016 Science

[3] Platz et al., 2016, in preparation

[4] Ruesch et al., 2016, Science