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How did the dwarf galaxy population of present-day galaxy clusters form andgrow over time? We address this question by analysing the history of darkmatter subhaloes in the Millennium-II cosmological simulation. A semi-analyticmodel serves as the link to observations. We argue that a reasonable analogueto early morphological types or red-sequence dwarf galaxies are those subhaloesthat experienced strong mass loss, or alternatively those that have spent along time in massive haloes. This approach reproduces well the observedmorphology-distance relation of dwarf galaxies in the Virgo and Coma clusters,and thus provides insight into their history. Over their lifetime, present-daylate types have experienced an amount of environmental influence similar towhat the progenitors of dwarf ellipticals had already experienced at redshiftsabove two. Therefore, dwarf ellipticals are more likely to be a result of earlyand continuous environmental influence in group- and cluster-size haloes,rather than a recent transformation product. The observed morphologicalsequences of late-type and early-type galaxies have developed in parallel, notconsecutively. Consequently, the characteristics of today's late-type galaxiesare not necessarily representative for the progenitors of today's dwarfellipticals. Studies aiming to reproduce the present-day dwarf population thusneed to start at early epochs, model the influence of various environments, andalso take into account the evolution of the environments themselves.

Dwarf galaxy populations in present-day galaxy clusters - II. The history of early-type and late-type dwarfs