  It is shown that globular clusters and the dwarf spheroidal companions of the
Galaxy have a different distribution of flattening values, and appear to occupy
adjacent regions of the M_v versus log R_h plane that can be separated by what
will be referred to as the Shapley line. Surprisingly, typical dwarf spheroidal
companions to the Milky Way System are fainter than the average Galactic
globular cluster.
