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We present new results from our comprehensive comparative survey of twomassive, intermediate redshift galaxy clusters, Cl0024+17 (z=0.39) andMS0451-03 (z=0.54). We identify and study several key classes of `transitionobjects' whose stellar populations or dynamical states indicate a recent orongoing change in morphology and star formation rate. For the first time, wehave been able to conclusively identify spiral galaxies in the process oftransforming into S0 galaxies. This has been accomplished by locating bothspirals whose star formation is being quenched as well as their eventualsuccessors, the recently created S0s. Differences between the two clusters inboth the timescales and spatial location of this conversion process allow us toevaluate the relative importance of several proposed physical mechanisms thatcould be responsible for the transformation. Combined with other diagnosticsthat are sensitive to either ICM-driven galaxy evolution or galaxy-galaxyinteractions, we describe a self-consistent picture of galaxy evolution inclusters. We find that spiral galaxies within infalling groups have alreadybegun a slow process of conversion into S0s primarily via gentle galaxy-galaxyinteractions. The fates of spirals upon reaching the core of the cluster dependheavily on the cluster ICM, with rapid conversion of all remaining spirals intoS0s via ram-pressure stripping in clusters where the ICM is dense. In thepresence of a less-dense ICM, the conversion continues at a slower pace, withgalaxy-galaxy interactions continuing to play a role along with `starvation' bythe ICM. We conclude that the buildup of the local S0 population through thetransformation of spiral galaxies is a heterogeneous process that neverthelessproceeds robustly across a variety of different environments.

A Wide-field Survey of Two Z~0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s