skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: THE CFHTLS-DEEP CATALOG OF INTERACTING GALAXIES. I. MERGER RATE EVOLUTION TO z = 1.2

Journal Article · · Astrophysical Journal
 [1]; ;  [2]
  1. California Institute of Technology, Pasadena, CA 91125 (United States)
  2. University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4 (Canada)

We present the rest-frame optical galaxy merger fraction between 0.2 < z < 1.2, as a function of stellar mass and optical luminosity, as observed by the Canada-France-Hawaii Telescope Legacy Deep Survey (CFHTLS-Deep). We developed a new classification scheme to identify major galaxy-galaxy mergers based on the presence of tidal tails and bridges. These morphological features are signposts of recent and ongoing merger activity. Through the visual classification of all galaxies, down to i{sub vega} <= 22.2 (approx27,000 galaxies) over 2 square degrees, we have compiled the CFHTLS-Deep Catalog of Interacting Galaxies, with approx 1600 merging galaxies. We find the merger fraction to be 4.3% +- 0.3% at z approx 0.3 and 19.0% +- 2.5% at z approx 1, implying evolution of the merger fraction going as (1 + z) {sup m}, with m = 2.25 +- 0.24. This result is inconsistent with a mild or non-evolving (m < 1.5) scenario at a approx>4sigma level of confidence. A mild trend, where by massive galaxies with M{sub *}>10{sup 10.7} M{sub sun} are undergoing fewer mergers than less massive systems (M{sub *} approx 10{sup 10} M{sub sun}), consistent with the expectations of galaxy assembly downsizing is observed. Our results also show that interacting galaxies have on average SFRs double that found in non-interacting field galaxies. We conclude that (1) the optical galaxy merger fraction does evolve with redshift, (2) the merger fraction depends mildly on stellar mass, with lower mass galaxies having higher merger fractions at z < 1, and (3) star formation is triggered at all phases of a merger, with larger enhancements at later stages, consistent with N-body simulations.

OSTI ID:
21392286
Journal Information:
Astrophysical Journal, Vol. 709, Issue 2; Other Information: DOI: 10.1088/0004-637X/709/2/1067; ISSN 0004-637X
Country of Publication:
United States
Language:
English