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Lunar surface properties at both polar and equatorial regions were studied using data from the miniaturized synthetic aperture radar (Mini-SAR) on-board Chandrayaan-1. The Mini-SAR sensor was operated at the S-band (2.38 GHz) with left circular polarization for transmission, and horizontal and vertical polarizations for reception. The returned signal was stored in planetary data system format, where each pixel in an image strip was represented by the corresponding Stokes vectors. The study showed that circular polarization ratio, which is an important parameter that represents scattering associated with planetary ice as well as dihedral reflection, was anomalously high inside some of the craters in the polar regions. Other Stokes parameters such as degree of polarization (m) and LH-LV relative phase (δ) also showed distinctly different types of scattering mechanisms inside and outside the craters on the lunar surface. [ABSTRACT FROM AUTHOR]

The surface layer of the Moon preserves vital evidences of lunar impact and cratering processes due to the absence of any Aeolian and fluvial erosion processes acting on it. By examining these evidences, which are recorded throughout the evolutionary history of the Moon, several basic aspects of lunar science can be understood, and this has direct relevance to the surfaces of other airless bodies within the solar system. In this study, rock abundance data obtained from Thermal Infrared (TIR) observations and radar Circular Polarization Ratio (CPR) data sets obtained from polarimetric SAR observations were correlated at some sample sites on the lunar surface. Preliminary results yielded qualitative and quantitative estimates for surface rock abundances. Except at distal ejecta deposits of young, bright craters a general correlation was observed between the two datasets. Mixed results were observed from the impact melt flows where the situation is complex due to the possible subsurface-volume and volume-subsurface interactions of the radar waves. But the flow features were clearly separated from the interior and ejecta regions of their parent craters in terms of CPR and rock abundances. The extent and distributions of pyroclastic deposits and dark haloed regions could not be distinctly identified at the resolution of datasets utilized. Near Gerasimovich D crater, the Diviner Radiometer has provided the first TIR observations of a newly discovered impact melt flow which was not visible in the optical imagery. This facilitated the first ever quantitative comparisons of the radar CPR and rock abundance values near such a region. Also, significant differences in spatial patterns between the radar and rock concentration data sets were observed, owing to the differences in the sensitivity of the two observations. [ABSTRACT FROM AUTHOR]