One of the more astonishing results of the LCROSS mission were spectra indicating large concentrations of native precious metals. We hypothesize that the reported metal concentrations represent electrostatic placer deposits: we theorize that electrostatic dust transport preferentially favors transport of submicron-sized native metal particles that get trapped in permanently shadowed regions (PSRs) within much smaller subareas where solar wind wake effects are minimal. We review the LRO LAMP and SSC UV/VIS data and note that several spectral emission lines in the UV are consistent with the presence of platinum, as well as silver and gold. We also conduct a numerical simulation that shows that levitation of submicron-sized gold particles is favored compared with dielectric dust particles. We then develop an ore genesis model that predicts a soil mass abundance of 0.11% for Au within the ore body trap that is in rough agreement with the estimate of 0.52% for Au based on the LRO LAMP column density observations. We apply the same methodology to Hg, and predict a soil mass abundance of 0.53% Hg, compared with an estimated 0.39% Hg based on LRO LAMP column densities.Greenfield ore grades are determined initially by remote sensing techniques and ore body genesis modeling; secondly by exploratory drilling and sampling; and finally by close-in ore body delineation (detailed sampling and analysis) to provide a 3D picture of the ore body of interest. Now that we have in hand a large body of various remote sensing data sets, and a predictive ore genesis model, we propose to undertake the second stepexploratory drilling. Since the occurrence of electrostatic placer deposits tends to coincide with deposits of volatiles, the upcoming Resource Prospector Mission (RPM) will be in an ideal position to detect native precious metals as well as volatiles. However, the Lunar Advanced Volatile Analysis (LAVA) instrument can only characterize volatiles below 70 AMU, whereas Ag, Pt, Au, and Hg atoms range in mass from 108 to 200 AMU. Therefore, we propose that an "X-Ray Spectrometer System" (XSS) be added to the RPM rover as a secondary scientific payload. The XSS instrument will primarily consist of an X-ray fluorescence detector (XRF) that offers the right combination of low mass, low power requirements, high speed, and high accuracy (ppm level for heavy precious metals). Finally, since water derived from PSRs will eventually be intended for human consumption, the likely high concentration of Hg in PSRs is a potentially grave health hazard, and represents a huge knowledge gap in our understanding of how to work and live on the lunar surface that is left unaddressed by the RPM in its present configuration. Nomenclature η = photoelectric efficiency ϕ = dust particle surface potential a = cross sectional area of dust particle Ai = area of source terrain i Downloaded by MONASH UNIVERSITY on August 1, 2015 | http://arc.aiaa.org | 2 Atrap = area of mineral resource trap Ci = mineral concentration of source terrain i Core = mineral concentrat...

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