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. Author manuscript; available in PMC: 2019 Mar 6.
Published in final edited form as: Rev Mineral Geochem. 2016 Jan 1;81(1):161–238. doi: 10.2138/rmg.2016.81.04

Figure 6.

Figure 6.

Os concentration (pg.g−1) versus 187Os/188Os for lunar pristine crustal rocks, lunar impact-melt breccias (LIMB; Puchtel et al. 2008) and chondrites (Horan et al. 2003) versus data for six eucrite falls (unpublished data of first author) and eucrites from Dale et al. (2012). Curve shows mixing between a hypothetical pristine ferroan anorthosite [FAN] lunar crust composition (represented by large aliquants of Apollo FAN 60025: 187Os/188Os = ~0.22; Os = 1 pg.g−1) and average chondrite composition (187Os/188Os = 0.1275; Os = 840,000 pg.g−1). Percentages (by mass) of the chondritic component are labeled. Note that the Os concentration data are logarithmic. Elevated HSE abundances and near-chondritic 187Os/188Os of some magnesian suite [MGS] samples (e.g., 77215, 78235) and Pasamonte, most likely indicate traces of meteoritic contamination.