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We derive deep $I$ band luminosity functions and colour-magnitude diagramsfrom HST imaging for eleven $0.2<z<0.6$ clusters observed at various stages ofmerging, and a comparison sample of five more relaxed clusters at similarredshifts. The characteristic magnitude $M^*$ evolves passively out to $z=0.6$,while the faint end slope of the luminosity function is $\alpha \sim -1$ at allredshifts. Cluster galaxies must have been completely assembled down to $M_I\sim -18$ out to $z=0.6$. We observe tight colour-magnitude relations over aluminosity range of up to 8 magnitudes, consistent with the passive evolutionof ancient stellar populations. This is found in all clusters, irrespective oftheir dynamical status (involved in a collision or not, or even withinsubclusters for the same object) and suggests that environment does not have astrong influence on galaxy properties. A red sequence luminosity function canbe followed to the limits of our photometry: we see no evidence of a weakeningof the red sequence to $z=0.6$. The blue galaxy fraction rises with redshift,especially at fainter absolute magnitudes. We observe bright blue galaxies inclusters at $z > 0.4$ that are not encountered locally. Surface brightnessselection effects preferentially influence the detectability of faint redgalaxies, accounting for claims of evolution at the faint end.

Deep Luminosity Functions and Colour-Magnitude Relations for Cluster Galaxies at 0.2 < z < 0.6