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We have obtained new CCD photometry for a sample of $\simeq 800$ early-typegalaxies (dwarf and giant ellipticals) in the central 700 arcmin$^2$ of theComa 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 allgalaxies in the cluster core (excluding NGC 4874 and NGC 4889) is modeled asthe sum of a Gaussian distribution for the giant galaxies and a Schechterfunction for the dwarf elliptical galaxies. We determine that the early-typedwarf-to-giant ratio (EDGR) for Coma is identical to that measured for the lessrich Virgo cluster; i.e., the EDGR does not increase as predicted by theEDGR-richness correlation. We postulate that the presence of substructure is animportant factor in determining the cluster's EDGR; that is, the EDGR for Comais consistent with the Coma cluster being built up from the merger of multipleless-rich galaxy clusters.

The Early-Type Dwarf-to-Giant Ratio and Substructure in the Coma Cluster