The author has previously suggested that shergottites and possibly other SNC meteorites were launched from the Martian surface by the oblique impact of large meteoroids. This hypothesis is further evaluated in the context of the subsequent discovery of a lunar meteorite. The oblique impact hypothesis is consistent with observations concerning the lunar and putative Martian meteorites. Obliue impacts are comparatively rare consistent with the observation that ejecta from only one lunar event and one or two putative Martian events have been recognized. The hypothesis is also consistent with the observation of ejecta from a more volatile-enriched object, Mars. Furthermore, in spite of the comparative rarity of oblique impacts, there exists at least one candidate source crater for the lunar meteorite in the lunar highlands adjacent to a source of the VLT basalt fragment discovered in it. There also exist at least two candidate source craters on Martian terrain of appropriate age to be the source terrain of the SNC meteorites. The candidate source craters are of appropriate size to be representative of events that have contributed to the current inventory of a continuous background of space stored lunar and Marrtian ejecta. Finally, it is shown that within calculational uncertainities and the current poorly known fall statistics of lunar and probable Martian meteorites, the oblique impact hypothesis gives a satisfactory explanation of the relative abundances of lunar, Martian, and other meteorites. These results support the oblique-impact-on-Mars origin of SNC meteorites and give a satisfactory explanation for the occurence of lunar meteorite.