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To study systematically the evolution on the angular extents of the galaxy,ICM, and dark matter components in galaxy clusters, we compiled the optical andX-ray properties of a sample of 340 clusters with redshifts $<0.5$, based onall the available data with the Sloan Digital Sky Survey (SDSS) and {\itChandra}/{\it XMM-Newton}. For each cluster, the member galaxies weredetermined primarily with photometric redshift measurements. The radial ICMmass distribution, as well as the total gravitational mass distribution, werederived from a spatially-resolved spectral analysis of the X-ray data. Whennormalizing the radial profile of galaxy number to that of the ICM mass, therelative curve was found to depend significantly on the cluster redshift; itdrops more steeply towards outside in lower redshift subsamples. The sameevolution is found in the galaxy-to-total mass profile, while the ICM-to-totalmass profile varies in an opposite way. We interpret that the galaxies, theICM, and the dark matter components had similar angular distributions when acluster was formed, while the galaxies travelling interior of the cluster havecontinuously fallen towards the center relative to the other components, andthe ICM has slightly expanded relative to the dark matter although it suffersstrong radiative loss. This cosmological galaxy infall, accompanied by an ICMexpansion, can be explained by considering that the galaxies interact stronglywith the ICM while they are moving through it. The interaction is considered tocreate a large energy flow of $10^{44-45}$ erg $\rm s^{-1}$ per cluster fromthe member galaxies to their environment, which is expected to continue overcosmological time scales.

Galaxy Infall by Interacting with its Environment: a Comprehensive Study of 340 Galaxy Clusters