Six lunar meteorites have thus far been discovered in Antarctica. Although these meteorites are of undocumented lunar-geographic provenance, all other available lunar samples (obtained from the Apollo and Luna programs) came from a relatively minuscule region of the central nearside, around which a polygon could be drawn covering just 4.7% of the lunar surface. The five lunar meteorites that are now well-studied represent at least two but probably three separate lunar source craters: ALHA81005 and Y791197 are probably from separate craters, and compound meteorite Y82192/6032 is certainly from a crater of its own. At least ALHA81005 and Y791197, and probably also (at least in a loose sense) Y82192/6032, are highlands regolith breccias. Thus, their compositions may be appropriately compared with compositions of Apollo and Luna highlands regolith samples. Compared with average highlands regolith samples from the central nearside Apollo sites, lunar meteorites have lower concentrations of siderophile elements in general, and especially Au, Ge and Ni. Among anorthositic Apollo samples (i.e., mainly those from Apollo 16), Au/Ir and to a lesser extent Ge/Ir ratios tend to be hyperchondritic. Most previous models for lunar regolith siderophile geochemistry assumed that the Apollo 16 samples are representative of the overall lunar highlands. Such models tended to conclude that the hyperchondritic Au/Ir and Ge/Ir ratios were consequences of variations in the compositions of Moon-striking projectiles as a function of time. It was even speculated that these temporal variations were consequences of the heterogeneous accretion of a Moon with a general enrichment in refractory elements. The lunar meteorites suggest that hyperchondritic Au/Ir and Ge/Ir are not general features of the highlands, but peculiarities of the Apollo 16 region, or more generally, the central nearside. The high Ni contents of the Apollo 16 megaregolith, substantially in excess of the Ni implied by a model in which all meteoritic debris has an H-chondritic Ni/Ir ratio, have been interpreted to imply that the Mg-rich fraction of the lunar crust is extremely Ni-rich, and thus similar in siderophile geochemistry to terrestrial komatiites. This coincidence has been interpreted as confirmation that the Moon formed by modified fission from the Earth's mantle, after core formation (plus late-accretion effects) had established the final siderophile pattern of the Earth's mantle. However, the lunar meteorites (and a survey of data for the Luna 20 highlands regolith sample) suggest that the high Ni content of the Apollo 16 regolith is strictly a peculiarity of the Apollo 16 region, and not a general feature of the Moon's crust. The anomalous siderophile composition of the central nearside regolith probably stems from a combination of regional heterogeneity in cratering-projectile compositions, plus regional enrichments in relatively “labile” siderophile elements (most notably Au, Ge, and perhaps to a certain extent Ni), which might be loosely correlated with the anomalously high concentration of KREEP over the central nearside.