One important approach to the study of galaxy evolution is to identify those galaxies whose spectral and/or morphological characteristics suggest that they are in transition. For example, ``E+A galaxies, which have strong Balmer absorption lines and no significant [OII] emission, are generally interpreted as post-starburst galaxies in which the star formation ceased within the last Gyr. This transition between a star forming and non-star forming state is a critical link in any galaxy evolution model in which a blue, star forming disk galaxy evolves into a S0 or elliptical. Another possible evolutionary track is that the star formation in an ``E+A resumes at some later time, if enough gas remains in the galaxy after its starburst ends. Given this ambiguity, it is important to investigate (1) the environments role in ``E+A evolution, (2) the stellar and gas morphologies of ``E+As, (3) the likely progenitors of ``E+As, and (4) how common the ``E+A phase is in the evolution of galaxies. This proceeding summarizes recent results from several inter-related projects designed to address these questions. These projects focus on a sample of 21 nearby ``E+A galaxies (0.05 < z < 0.15) drawn from the Las Campanas Redshift Survey. These studies include VLA and HST observations, in addition to comparisons of these data with galaxy-galaxy interaction simulations and stellar population synthesis models.
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