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We combine a N-body simulation algorithm with a subgrid treatment of galaxyformation, mergers, and tidal destruction, and an observed conditionalluminosity function Phi(L|M), to study the origin and evolution of galactic andextragalactic light inside a cosmological volume of size (100 Mpc)^3, in aconcordance LCDM model. This algorithm simulates the growth of large-scalestructures and the formation of clusters, the evolution of the galaxypopulation in clusters, the destruction of galaxies by mergers and tides, andthe evolution of the intracluster light. We find that destruction of galaxiesby mergers dominates over destruction by tides by about an order of magnitudeat all redshifts. However, tidal destruction is sufficient to produceintracluster light fractions f_ICL that are sufficiently high to matchobservations. The bulk of the intracluster light (60%) is provided byintermediate galaxies of total masses 10^11 Msun-10^12 Msun and stellar masses6x10^8 Msun-3x10^10 Msun that were tidally destroyed by even more massivegalaxies. The contribution of low-mass galaxies to the intracluster light issmall and the contribution of dwarf galaxies is negligible, even though, bynumbers, most galaxies that are tidally destroyed are dwarfs. Tracking clustersback in time, we find that their values of f_ICL tend to increase over time,but can experience sudden changes that are sometimes non-monotonic. Thesechanges occur during major mergers involving clusters of comparable masses butvery different intracluster luminosities. Most of the tidal destruction eventstake place in the central regions of clusters. As a result, the intraclusterlight is more centrally concentrated than the galactic light. Our resultssupport tidal destruction of intermediate-mass galaxies as a plausible scenariofor the origin of the intracluster light.

The Fate of Dwarf Galaxies in Clusters and the Origin of Intracluster Stars. II. Cosmological Simulations