{
  "id": "1612.07322",
  "version": "v1",
  "published": "2016-12-21T21:00:02.000Z",
  "updated": "2016-12-21T21:00:02.000Z",
  "title": "Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies in the Local Universe I. - The Effect of the Group Environment on Star Formation in Spiral Galaxies",
  "authors": [
    "M. W. Grootes",
    "R. J. Tuffs",
    "C. C. Popescu",
    "P. Norberg",
    "A. S. G. Robotham",
    "J. Liske",
    "E. Andrae",
    "I. K. Baldry",
    "M. Gunawardhana",
    "L. S. Kelvin",
    "B. F. Madore",
    "M. Seibert",
    "E. N. Taylor",
    "M. Alpaslan",
    "M. J. I. Brown",
    "M. E. Cluver",
    "S. P. Driver",
    "J. Bland-Hawthorn",
    "B. W. Holwerda",
    "A. M. Hopkins",
    "A. R. Lopez-Sanchez",
    "J. Loveday",
    "M. Rushton"
  ],
  "comment": "Accepted for publication in AJ; 40 pages, 27 figures (8 full page), 6 tables, 5 appendices (10 pages), data in figures available in machine readable format from journal (or author on demand)",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "Abridged - We quantify the effect of the galaxy group environment (for 12.5 < log(M_group/Msun) < 14.0) on the star formation rates of the (morphologically-selected) population of disk-dominated local Universe spiral galaxies (z < 0.13) with stellar masses log(M*/Msun) > 9.5. Within this population, we find that, while a small minority of group satellites are strongly quenched, the group centrals, and the large majority of satellites exhibit levels of SFR indistinguishable from ungrouped \"field\" galaxies of the same M*, albeit with a higher scatter, and for all M*. Modelling these results, we deduce that disk-dominated satellites continue to be characterized by a rapid cycling of gas into and out of their ISM at rates similar to those operating prior to infall, with the on-going fuelling likely sourced from the group intrahalo medium (IHM) on Mpc scales, rather than from the circum-galactic medium on 100kpc scales. Consequently, the color-density relation of the galaxy population as a whole would appear to be primarily due to a change in the mix of disk- and spheroid-dominated morphologies in the denser group environment compared to the field, rather than to a reduced propensity of the IHM in higher mass structures to cool and accrete onto galaxies. We also suggest that the inferred substantial accretion of IHM gas by satellite disk-dominated galaxies will lead to a progressive reduction in their specific angular momentum, thereby representing an efficient secular mechanism to transform morphology from star-forming disk-dominated types to more passive spheroid-dominated types.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-12-21T21:00:02.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "spiral galaxies",
      "star formation",
      "local universe",
      "gas fuelling",
      "mass assembly"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 40,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}