Information about the variability,and spatial distribution of iron abundance is important to understand lunar geological history and for future resource utilization. In this paper we present a preliminary model to produce an iron abundance map using images taken by an Imaging Interferometer on board the satellite Chang'E-1. Compared with the Clementine UVVIS images,the images from the Chang'E-1 satellite also allowed for the extraction of FeO abundance distributions on the Moon. However,the prelimi-nary model results suggest an underestimation of ～2 wt.% for the FeO content of the mare region and an overestimation of ～3 wt.% for the highland region.
The distribution of titanium abundance on the lunar surface is important knowledge for lunar geologic studies and future resource utilization.In this paper,we develop a preliminary model based on"ground truths"from Apollo and Luna sample-return sites to produce a titanium abundance map from Chang’E-1 Imaging Interferometer(IIM) images.The derived TiO2 abundances are validated with Clementine UVVIS results in several regions,including lunar highlands neighboring the Apollo 16 landing site,and high-Ti and low-Ti maria near the standard site of Mare Serenitatis(MS2) .The validation results show that TiO2 abundances modeled with Chang’E-1 IIM data are overestimated for highlands(～0.7 wt.%) and low-Ti maria(～1.5 wt.%) and underestimated for high-Ti maria(～0.8 wt.%).
A systematic spectroscopic study including Raman, Mid-IR, N1R, and VIS-NIR, is used to investigate four endmember lunar soils. Apollo soils （〈45 μm） 14163, 15271, 67511, and 71501 were selected as endmembers to study, based on their soil chemistry, maturity against space weathering, and the sampling locations. These endmembers include an anorthositic highlands soil （67511）, a low-Ti basaltic soil （15271）, a high-Ti basaltic soil （71501）, and a mafic, KREEPy, impact-melt-rich soil （14163）. We used a laser Raman point-counting procedure to derive mineral modes of the soils and the compositional distributions of major mineral phases, which in turn reflect characteristics of the main source materials for these soils. The Mid-IR, NIR, and VIS-NIR spectroscopic properties also yield distinct information on mineralogy, geochemistry, and maturity among the four soils. Knowledge of the mineralogy resulting from the Raman point-counting procedure corresponds well with bulk mineralogy and soil properties based on Mid-IR, NIR, and VIS-NIR spectroscopy. The future synergistic application of these spectroscopy methods on the Moon will provide a linkage between the results from in situ surface exploration and those from orbital remotesensing observations.
