  We have obtained new CCD photometry for a sample of $\simeq 800$ early-type
galaxies (dwarf and giant ellipticals) in the central 700 arcmin$^2$ of the
Coma cluster, complete in color and in magnitude to $R = 22.5$ mag ($M_R \simeq
-12$ mag for $H_0 = 86$ km/sec/Mpc). The composite luminosity function for all
galaxies in the cluster core (excluding NGC 4874 and NGC 4889) is modeled as
the sum of a Gaussian distribution for the giant galaxies and a Schechter
function for the dwarf elliptical galaxies. We determine that the early-type
dwarf-to-giant ratio (EDGR) for Coma is identical to that measured for the less
rich Virgo cluster; i.e., the EDGR does not increase as predicted by the
EDGR-richness correlation. We postulate that the presence of substructure is an
important factor in determining the cluster's EDGR; that is, the EDGR for Coma
is consistent with the Coma cluster being built up from the merger of multiple
less-rich galaxy clusters.
