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By tracing the orbital and star formation histories of galaxies within theComa cluster, we seek to understand the role of the high-density clusterenvironment in quenching these galaxies. We combine star formation historiesextracted from high-signal-to-noise spectra of 11 early-type galaxies aroundthe center of the Coma cluster with probability distributions for their orbitalparameters obtained using an N-body simulation to connect their orbital andstar formation histories. We find that all 11 galaxies likely quenched neartheir first pericentric approach. Higher stellar mass galaxies($\log(M_\star/\mathrm{M}_\odot)>10$) had formed a higher fraction of theirstellar mass (more than $\sim90\%$) than their lower mass counterparts ($\sim80$-$90\%$) by the time they fell into the cluster (when they cross$2.5r_\mathrm{vir}$). We find that the expected infall occurred around$z\sim0.6$, followed by the first pericentric passage $\sim4\,\mathrm{Gyr}$later. Galaxies in our sample formed a significant fraction of their stellarmass, up to $15\%$, between infall and first pericenter, and had assembled morethan $\sim98\%$ of their cumulative stellar mass by first pericenter. Unlikeprevious low-redshift studies that suggest that star formation continues untilabout first apocenter or later, the high percentage of stellar mass alreadyformed by first pericenter in our sample galaxies points to star formationceasing within a gigayear after the first pericentric passage. We consider thepossible physical mechanisms driving quenching and find that our resultsresemble the situation in clusters at $z\sim1$, where active stripping of gas(ram-pressure or tidally driven) seems to be required to quench satellites bytheir first pericentric passage. However, a larger sample will be required toconclusively account for the unknown fraction of preprocessed satellites in theComa cluster.

Star formation histories of Coma Cluster galaxies matched to simulated orbits hint at quenching around first pericenter