Photometric Modeling and VIS‐IR Albedo Maps of Dione From Cassini‐VIMS. Issue 5 (15th March 2018)

• Record Type: Journal Article
• Authors: Filacchione, G.; Ciarniello, M.; D'Aversa, E.; Capaccioni, F.; Cerroni, P.; Buratti, B. J.; Clark, R. N.; Stephan, K.; Plainaki, C.
• Is Part Of: Geophysical research letters. Volume 45:Issue 5(2018)
• Page Start: 2184
• Page End: 2192
• Publication Date: 2018-03-15
• Subjects: Dione -- photometric correction -- phase function -- albedo maps -- water ice band depth map -- Cassini/VIMS; Geophysics -- Periodicals; Planets -- Periodicals; Lunar geology -- Periodicals; 550
• DOI: 10.1002/2017GL076869
• Languages: English
• ISSNs: 0094-8276

Abstract

Abstract: We report about visible and infrared albedo maps and spectral indicators of Dione's surface derived from the complete Visual and Infrared Mapping Spectrometer (VIMS) data set acquired between 2004 and 2017 during the Cassini tour in Saturn's system. Maps are derived by applying a photometric correction necessary to disentangle the intrinsic albedo of the surface from illumination and viewing geometry occurring at the time of the observation. The photometric correction is based on the Shkuratov et al. (2011, https://doi.org/10.1016/j.pss.2011.06.011 ) method which yields values of the surface equigonal albedo. Dione's surface albedo maps are rendered at five visible (VIS: 0.35, 0.44, 0.55, 0.7, and 0.95 μm) and five infrared (IR: 1.046, 1.540, 1.822, 2.050, and 2.200 μm) wavelengths in cylindrical projection with a 0.5° × 0.5° angular resolution in latitude and longitude, corresponding to a spatial resolution of 4.5 km/bin. Apart from visible and infrared albedo maps, we report about the distribution of the two visible spectral slopes (0.35–0.55 and 0.55–0.95 μm) and water ice 2.050 μm band depth computed after having applied the photometric correction. The derived spectral indicators are employed to trace Dione's composition variability on both global and local scales allowing to study the dichotomy between the bright‐leading and dark‐trailing hemispheres, the distribution of fresh material on the impact craters and surrounding ejecta, and the resurfacing of the bright material within the chasmata caused by tectonism. Key Points: Application of photometric correction to Cassini‐VIMS data Computation of Dione albedo maps at VIS and IR wavelengths Retrieval of VIS slopes and water ice band depth maps