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Present-day clusters are massive halos containing mostly quiescent galaxies,while distant protoclusters are extended structures containing numerousstar-forming galaxies. We investigate the implications of this fundamentalchange in a cosmological context using a set of N-body simulations andsemi-analytic models. We find that the fraction of the cosmic volume occupiedby all (proto)clusters increases by nearly three orders of magnitude from z=0to z=7. We show that (proto)cluster galaxies are an important, and evendominant population at high redshift, as their expected contribution to thecosmic star-formation rate density rises (from 1% at z=0) to 20% at z=2 and 50%at z=10. Protoclusters thus provide a significant fraction of the cosmicionizing photons, and may have been crucial in driving the timing and topologyof cosmic reionization. Internally, the average history of cluster formationcan be described by three distinct phases: at z~10-5, galaxy growth inprotoclusters proceeded in an inside-out manner, with centrally dominant halosthat are among the most active regions in the Universe; at z~5-1.5, rapid starformation occurred within the entire 10-20 Mpc structures, forming most oftheir present-day stellar mass; at z<~1.5, violent gravitational collapse drovethese stellar contents into single cluster halos, largely erasing the detailsof cluster galaxy formation due to relaxation and virialization. Our resultsmotivate observations of distant protoclusters in order to understand therapid, extended stellar growth during Cosmic Noon, and their connection toreionization during Cosmic Dawn.

Galaxy Protoclusters as Drivers of Cosmic Star-Formation History in the First 2 Gyr