^1,2Xiaojia Zeng, ¹Xiongyao Li, ¹Shijie Wang, ¹Shijie Li, ³Nicole Spring, ¹Hong Tang, ¹Yang Li, ¹Junming Feng
¹Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 55002, China
²University of Chinese Academy of Sciences, Beijing 10049, China
³School of Earth, Atmospheric and Environmental Sciences, University of Manchester, Manchester, UK

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Reference
Zeng X, Li X, Wang S, Li S, Spring N, Tang H, Li Y, Feng J (2015) JMSS-1: a new Martian soil simulant.
Earth, Planets and Space 67:72
Link to Article [doi:10.1186/s40623-015-0248-5]

¹E. Ammannito
¹University of California Los Angeles, Earth Planetary and Space Sciences, Los Angeles, CA-90095, USA
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We present and describe the maps of spectral parameters such as pyroxene band centers and depths, reflectance at 1.4 μm and 2.8μm band depth in the Rheasilvia quadrangle. We found a broad anti-correlation between pyroxene band centers and depths while the reflectance is not correlated with the pyroxene spectral parameters. In addition, we found that the Rheasilvia quadrangle is free of OH absorption signatures. We also derived lithological maps with improvements in the spatial resolution with respect to previous lithological maps of the same region. We confirm that the central mound is dominated by eucritic/howarditic pyroxene while diogenitic lithology has been found mainly in a region delineated by Tarpeia, Severina and Mariamne craters. We found small scale variations in the composition of pyroxene. These variations identify lithological units that extend for tens of km, although small units of less than 1 km have also been found. We consider this fact as an indication of a high level of compositional heterogeneity within the Vestan crust.

Reference
Ammannito E et al. (2015) Compositional variations in the Vestan Rheasilvia basin. Icarus (in Press)
Link to Article [doi:10.1016/j.icarus.2015.05.017]

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