The Detailed Evolution of E+A Galaxies into Early Types
Yujin Yang (1), Ann Zabludoff (1), Dennis Zaritsky (1), Christopher, Mihos (2) ((1) Steward Observatory, University of Arizona, (2) Case Western, Reserve University)

TL;DR
This study investigates the morphological and stellar population properties of E+A galaxies, revealing their similarities to early-type galaxies and supporting the idea that they are merger remnants evolving into early types.
Contribution
The paper provides detailed morphological analysis of E+A galaxies using HST images, linking their properties to merger-driven evolution into early-type galaxies.
Findings
E+A galaxies have large bulge fractions and high concentration indices.
Most E+As exhibit positive color gradients, indicating concentrated young stellar populations.
E+As have a lower mass-to-light ratio compared to E/S0 galaxies, and host young star clusters.
Abstract
Post-starburst, or E+A galaxies, are the best candidates for galaxies in transition from being gas-rich and star-forming to gas-poor and passively-evolving via galaxy-galaxy mergers. To determine what E+A galaxies become after their young stellar populations fade away, we present the detailed morphologies of 21 E+As using HST images. We find that E+As are similar to early types in that they have large bulge fractions (median B/T = 0.59), high Sersic index (n > 4), and high concentration indices (C > 4.3). The large fraction (70%) of E+As with positive color gradients (i.e., bluer nuclei) indicates that the young stellar populations are more concentrated than the old populations. We show that these positive color gradients can evolve into the negative gradients typical in E/S0s if the central parts of these galaxies are metal enhanced. E+A galaxies stand apart from the E/S0s in the…
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