Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-12-02
Astronomy and Astrophysics
Astrophysics
7 pages, 3 PS figures, LaTeX, uses crckapb.sty. To appear in proceedings of IAU Symp. 186, "Galaxy Interactions at Low and Hig
Scientific paper
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 environment's role in ``E+A'' evolution, (2) the stellar and gas morphologies of ``E+A''s, (3) the likely progenitors of ``E+A''s, 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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