{
  "id": "1710.02676",
  "version": "v1",
  "published": "2017-10-07T11:51:23.000Z",
  "updated": "2017-10-07T11:51:23.000Z",
  "title": "Galaxy evolution in the metric of the Cosmic Web",
  "authors": [
    "K. Kraljic",
    "S. Arnouts",
    "C. Pichon",
    "C. Laigle",
    "S. de la Torre",
    "D. Vibert",
    "C. Cadiou",
    "Y. Dubois",
    "M. Treyer",
    "C. Schimd",
    "S. Codis",
    "V. de Lapparent",
    "J. Devriendt",
    "H. S. Hwang",
    "D. Le Borgne",
    "N. Malavasi",
    "B. Milliard",
    "M. Musso",
    "D. Pogosyan",
    "M. Alpaslan",
    "J. Bland-Hawthorn",
    "A. H. Wright"
  ],
  "comment": "26 pages, 18 figures, 7 tables, accepted for publication in MNRAS",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "The role of the cosmic web in shaping galaxy properties is investigated in the GAMA spectroscopic survey in the redshift range $0.03 \\leq z \\leq 0.25$. The stellar mass, $u - r$ dust corrected colour and specific star formation rate (sSFR) of galaxies are analysed as a function of their distances to the 3D cosmic web features, such as nodes, filaments and walls, as reconstructed by DisPerSE. Significant mass and type/colour gradients are found for the whole population, with more massive and/or passive galaxies being located closer to the filament and wall than their less massive and/or star-forming counterparts. Mass segregation persists among the star-forming population alone. The red fraction of galaxies increases when closing in on nodes, and on filaments regardless of the distance to nodes. Similarly, the star-forming population reddens (or lowers its sSFR) at fixed mass when closing in on filament, implying that some quenching takes place. Comparable trends are also found in the state-of-the-art hydrodynamical simulation Horizon-AGN. These results suggest that on top of stellar mass and large-scale density, the traceless component of the tides from the anisotropic large-scale environment also shapes galactic properties. An extension of excursion theory accounting for filamentary tides provides a qualitative explanation in terms of anisotropic assembly bias: at a given mass, the accretion rate varies with the orientation and distance to filaments. It also explains the absence of type/colour gradients in the data on smaller, non-linear scales.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-10-07T11:51:23.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "galaxy evolution",
      "stellar mass",
      "specific star formation rate",
      "3d cosmic web features",
      "type/colour gradients"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 26,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}