{
  "id": "1703.06145",
  "version": "v1",
  "published": "2017-03-17T18:00:07.000Z",
  "updated": "2017-03-17T18:00:07.000Z",
  "title": "Revisiting the bulge-halo conspiracy I: Dependence on galaxy properties and halo mass",
  "authors": [
    "Francesco Shankar",
    "Alessandro Sonnenfeld",
    "Gary A. Mamon",
    "Kyu-Hyun Chae",
    "Raphael Gavazzi",
    "Tommaso Treu",
    "Benedikt Diemer",
    "Carlo Nipoti",
    "Stewart Buchan",
    "Mariangela Bernardi",
    "Ravi K. Sheth",
    "Marc Huertas-Company"
  ],
  "comment": "23 pages, 10 figures, 3 Appendices (with an extra 7 figures). ApJ, accepted. Main results in Figures 3, 5, 6, 8",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "We carry out a systematic investigation of the total mass density profile of massive (Mstar>2e11 Msun) early-type galaxies and its dependence on galactic properties and host halo mass with the aid of a variety of lensing/dynamical data and large mock galaxy catalogs. The latter are produced via semi-empirical models that, by design, are based on just a few basic input assumptions. Galaxies, with measured stellar masses, effective radii and S\\'{e}rsic indices, are assigned, via abundance matching relations, host dark matter halos characterized by a typical LCDM profile. Our main results are as follows: (i) In line with observational evidence, our semi-empirical models naturally predict that the total, mass-weighted density slope at the effective radius gamma' is not universal, steepening for more compact and/or massive galaxies, but flattening with increasing host halo mass. (ii) Models characterized by a Salpeter or variable initial mass function and uncontracted dark matter profiles are in good agreement with the data, while a Chabrier initial mass function and/or adiabatic contractions/expansions of the dark matter halos are highly disfavored. (iii) Currently available data on the mass density profiles of very massive galaxies (Mstar>1e12 Msun), with Mhalo>3e14 Msun, favor instead models with a stellar profile flatter than a S\\'{e}rsic one in the very inner regions (r<3-5 kpc), and a cored NFW or Einasto dark matter profile with median halo concentration a factor of ~2 or <1.3, respectively, higher than those typically predicted by N-body numerical simulations.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-03-17T18:00:07.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "galaxy properties",
      "bulge-halo conspiracy",
      "host halo mass",
      "initial mass function",
      "dependence"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 23,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}