Distribution of Olivine and Plagioclase around the lunar impact basins from Multiband Imager Data

The upper part of the moon is considered to be mainly composed of plagioclase, olivine and pyroxene which crystallized during the cooling process of Lunar Magma Ocean (LMO). However, the vertical structure of these minerals is still unclear (Snyder et al., 1991 and 1992, Taylor et al., 1982). Lateral distributions of these minerals on the lunar surface are important to reconstruct the vertical structure. Yamamoto et al., (2010, 2012) clarified the global distribution of olivine and plagioclase on the lunar surface by Spectral Profiler (SP) data onboard the lunar explorer SELENE/Kaguya. We intend to make more regional analysis in a specific area around a large basin, which is expected to covered with ejecta deposits from deep interior of the moon excavated by an impact. In this study, we analyzed Multiband Imager (MI) data onboard SELENE/Kaguya to clarify the local distribution of olivine and plagioclase around the Crisium basin where the existence of these minerals has been confirmed by the previous studies. MI performed more dense observations with a higher spatial resolution than SP. Therefore, MI data are suitable for detailed analysis in the specific area. Because of MI's lower spectral resolution than SP, our extraction criteria of the target minerals were defined by referring to the SP data of olivine and plagioclase extracted by Yamamoto et al., (2010, 2012). We obtained the excavation depth from the diameter size of the crater that mineral was confirmed and considered the vertical structure of the Crisium basin ejector layer.