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We illuminate the altered evolution of galaxies in clusters compared to thefield by tracking galaxies in the IllustrisTNG300 simulation as they enterisolated clusters of mass $10^{13} < M_{\rm 200, mean} / {\rm M}_\odot <10^{15}$ (at $z=0$). We demonstrate significant trends in galaxy propertieswith residence time (time since first infall) and that there is a population ofgalaxies that remain star-forming even many Gyrs after their infall. Bycomparing the properties of galaxies at their infall time to their propertiesat $z=0$, we show how scaling relations, like the stellar-to-halo mass ratio,shift as galaxies live in the cluster environment. Galaxies with a residencetime of 10 Gyr increase their stellar-to-halo mass ratio, by around 1 dex. Asmeasurements of the steepest slope of the galaxy cluster number density profile($R_{\rm st}$), frequently used as a proxy for the splashback radius, have beenshown to depend strongly on galaxy selection, we show how $R_{\rm st}$ dependson galaxy residence time. Using galaxies with residence times less than onecluster crossing time ($\approx 5$ Gyr) to measure $R_{\rm st}$ leads tosignificant offsets relative to using the entire galaxy population. Galaxiesmust have had the opportunity to `splash back' to the first caustic to traceout a representative value of $R_{\rm st}$, potentially leading to issues forgalaxy surveys using UV-selected galaxies. Our wok demonstrates that theevolution of cluster galaxies continues well into their lifetime in the clusterand departs from a typical field galaxy evolutionary path.

How time weathers galaxies: The temporal impact of the cluster environment on galaxy formation and evolution