Combe, Jean-PhilippeJean-PhilippeCombeRAPONI, AndreaAndreaRAPONITOSI, FedericoFedericoTOSIDE SANCTIS, MARIA CRISTINAMARIA CRISTINADE SANCTISCARROZZO, FILIPPO GIACOMOFILIPPO GIACOMOCARROZZOZAMBON, FrancescaFrancescaZAMBONAMMANNITO, ELEONORAELEONORAAMMANNITOHughson, Kynan H. G.Kynan H. G.HughsonNathues, AndreasAndreasNathuesHoffmann, MartinMartinHoffmannPlatz, ThomasThomasPlatzThangjam, GuneshwarGuneshwarThangjamSchorghofer, NorbertNorbertSchorghoferSchröder, StefanStefanSchröderByrne, ShaneShaneByrneLandis, Margaret E.Margaret E.LandisRuesch, OttavianoOttavianoRueschMcCord, Thomas B.Thomas B.McCordJohnson, Katherine E.Katherine E.JohnsonSingh, Sandeep MagarSandeep MagarSinghRaymond, Carol A.Carol A.RaymondRussell, Christopher T.Christopher T.Russell2020-12-212020-12-2120190019-1035http://hdl.handle.net/20.500.12386/29029H2O-rich materials are locally exposed at the surface of Ceres as discovered from infrared reflectance spectra of the Visible and InfraRed mapping spectrometer (VIR) of the Dawn mission. Nine locations on Ceres exhibit diagnostic absorption bands of the H<SUB>2</SUB>O molecule at 2.00, 1.65 and 1.28 μm. The detections are all consistent with H<SUB>2</SUB>O ice mixed with low-albedo components. All the reported H<SUB>2</SUB>O exposures occur at latitudes poleward of 30° in fresh craters near rim shadows, have a surface area < 7 km<SUP>2</SUP>, and are associated with one or more surface features such as a morphological flow or landslide, fractures, high albedo, or a pole-facing slope (one case is confirmed to be adjacent to persistent shadow). In four occurrences, these detections are associated with small (< 0.1 km<SUP>2</SUP>) high-albedo areas that can be recognized in high-resolution imagery (∼35 m/pixel) from the Framing Camera (FC). Since all these observations are compatible with an H<SUB>2</SUB>O-rich subsurface, the replenishment of surficial H<SUB>2</SUB>O likely comes from the ice that is present underneath. In four other occurrences, H<SUB>2</SUB>O is detected on walls and floors of fresh impact craters, either in the shadow or adjacent to shadows, which suggests that local thermodynamical conditions may also favor the concentration of H<SUB>2</SUB>O in these areas.STAMPAenArticle10.1016/j.icarus.2017.12.0082-s2.0-85040118667000455073800004https://www.sciencedirect.com/science/article/pii/S001910351730324X2019Icar..318...22CFIS/05 - ASTRONOMIA E ASTROFISICA