Size‐magnitude diagram for star clusters in VCC 798 (dots), Milky Way globular clusters (crosses), Milky Way old open clusters (diamonds), and the faint fuzzy selection box from Larsen & Brodie 2000 (dotted square). The VCC 798 catalog was statistically cleaned of background contamination, and photometry was transformed to M_V using the relations in the text and a distance of 16.5 Mpc. The dashed line represents a constant mean surface brightness, ﹩\mu _{V}=20﹩ mag arcsec⁻², below which most DSCs lie. The locus of GCs in VCC 798 match the GCs in the Milky Way with the exception of the low surface brightness Galactic halo GCs which would fall below our detection threshold (lower right). Most of the Milky Way old open clusters would also fall below our detection threshold. The brightest of these clusters, however, would have the sizes and magnitudes of DSCs in our sample. In the Galaxy, there is a deficit of objects in the DSC locus. The faint fuzzy region selects the more extended DSCs.