Do clusters contain a large population of dwarf galaxies?

Abstract

We analyze systematic effects in the determination of the galaxy luminosity function in clusters using a deep mock catalogue constructed from a numerical simulation of a hierarchical universe. The results indicate a strong tendency to derive a rising faint end ($α\lsim -1.5$) in clusters selected in two dimensions, using a galaxy catalogue constructed with a universal flat luminosity function with $α\simeq -1.0$. This is due to the projection effects inherent in catalogues of clusters constructed using 2 dimensional data. Many of the clusters found in 2d have no significant 3d counterparts, and most suffer from massive background contamination that cannot be corrected for by subtracting random offset fields. The luminosity function of high surface brightness galaxies in the field and within small groups follows a Schechter function with a fairly flat faint end slope, $n(L)\propto L^α$ with $α= -0.9$ to -1.2. On the contrary, observational studies of clusters constructed using Abell, EDCC and APM catalogues are systematically found to have steeper luminosity functions with $α= -1.4$ to -2.0. This may be attributed to projection effects rather than a dominant population of high surface brightness dwarf galaxies ($M\gsim M^*+2$) in clusters. It should be straighforward to confirm our results by measuring redshifts of these faint cluster galaxies.