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We use a large mosaic of HST WFPC2 images to measure the colors andmorphologies of 194 spectroscopically confirmed members of the rich galaxycluster CL1358+62 at z=0.33. We study the color-magnitude (CM) relation as afunction of radius in the cluster. The intrinsic scatter in the restframe B-VCM relation of the elliptical galaxies is very small: ~0.022 magnitudes. The CMrelation of the ellipticals does not depend significantly on the distance fromthe cluster center. In contrast, the CM relation for the S0 galaxies doesdepend on radius: the S0s in the core follow a CM relation similar to theellipticals, but at large radii (R>0.7Mpc) the S0s are systematically bluer andthe scatter in the CM relation approximately doubles to ~0.043 magnitudes. Theblueing of the S0s is significant at the 95% confidence level. These resultsimply that the S0 galaxies in the outer parts of the cluster have formed starsmore recently than the S0s in the inner parts. A likely explanation is thatclusters at z=0.33 continue to accrete galaxies and groups from the field andthat infall extinguishes star formation. The apparent homogeneity of theelliptical galaxy population implies that star formation in recently accretedellipticals was terminated well before accretion occurred. We have constructedmodels to explore the constraints that these observations place on the starformation history of cluster galaxies. We conclude that the population of S0sin clusters is likely to evolve as star forming galaxies are converted intopassively evolving galaxies. Assuming a constant accretion rate after z=0.33,we estimate ~15% of the present day early-type galaxy population in richclusters was accreted between z=0.33 and z=0. The ellipticals (and thebrightest S0s) are probably a more stable population, at least since z=0.6.

The Color‐Magnitude Relation in CL 1358+62 atz= 0.33: Evidence for Significant Evolution in the S0 Population