{
  "id": "1605.03182",
  "version": "v1",
  "published": "2016-05-10T20:00:01.000Z",
  "updated": "2016-05-10T20:00:01.000Z",
  "title": "Effects of Local Environment and Stellar Mass on Galaxy Quenching out to z~3",
  "authors": [
    "Behnam Darvish",
    "Bahram Mobasher",
    "David Sobral",
    "Alessandro Rettura",
    "Nick Scoville",
    "Andreas Faisst",
    "Peter Capak"
  ],
  "comment": "17 pages, 10 figures, Accepted for publication in the ApJ",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We study the effects of local environment and stellar mass on galaxy properties using a mass complete sample of quiescent and star-forming systems in the COSMOS field at $z\\lesssim$ 3. We show that at $z\\lesssim$ 1, the median star-formation rate (SFR) and specific SFR (sSFR) of all galaxies depend on environment, but they become independent of environment at $z\\gtrsim$ 1. However, we find that only for \\textit{star-forming} galaxies, the median SFR and sSFR are similar in different environments, regardless of redshift and stellar mass. We find that the quiescent fraction depends on environment at $z\\lesssim$ 1, and on stellar mass out to $z\\sim$ 3. We show that at $z\\lesssim$ 1, galaxies become quiescent faster in denser environments and that the overall environmental quenching efficiency increases with cosmic time. Environmental and mass quenching processes depend on each other. At $z\\lesssim$ 1, denser environments more efficiently quench galaxies with higher masses (log($M/M_{\\odot}$)$\\gtrsim$ 10.7), possibly due to a higher merger rate of massive galaxies in denser environments, and that mass quenching is more efficient in denser regions. We show that the overall mass quenching efficiency ($\\epsilon_{mass}$) for more massive galaxies (log($M/M_{\\odot}$)$\\gtrsim$ 10.2) rises with cosmic time until $z\\sim$ 1 and flattens out since then. However, for less massive galaxies, the rise in $\\epsilon_{mass}$ continues to the present time. Our results suggest that environmental quenching is only relevant at $z\\lesssim$ 1, likely a fast process, whereas mass quenching is the dominant mechanism at $z\\gtrsim$ 1, with a possible stellar feedback physics.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-05-10T20:00:01.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "stellar mass",
      "local environment",
      "galaxy quenching",
      "mass quenching",
      "denser environments"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 17,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}