Observational analysis of COSMOS galaxy groups shows quiescent fraction builds steadily from z~1.5-2 with faster growth in richer groups, first RS ridgeline galaxies by z~2, a possible early overdensity at z=3.4, and no significant evolution in RS slope or scatter.
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Merger-disturbed cluster galaxies remain bluer than undisturbed ones across all locations and morphologies, possibly because mergers trigger star formation or protect central gas from stripping.
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COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction
Observational analysis of COSMOS galaxy groups shows quiescent fraction builds steadily from z~1.5-2 with faster growth in richer groups, first RS ridgeline galaxies by z~2, a possible early overdensity at z=3.4, and no significant evolution in RS slope or scatter.
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Impact of Galaxy Mergers on the Colours of Cluster Galaxies
Merger-disturbed cluster galaxies remain bluer than undisturbed ones across all locations and morphologies, possibly because mergers trigger star formation or protect central gas from stripping.