{
  "id": "1807.00820",
  "version": "v1",
  "published": "2018-07-02T18:00:00.000Z",
  "updated": "2018-07-02T18:00:00.000Z",
  "title": "The stellar mass function of galaxies in Planck-selected clusters at 0.5 < z < 0.7: new constraints on the timescale and location of satellite quenching",
  "authors": [
    "Remco F. J. van der Burg",
    "Sean McGee",
    "Herve Aussel",
    "Hakon Dahle",
    "Monique Arnaud",
    "Gabriel W. Pratt",
    "Adam Muzzin"
  ],
  "comment": "16 pages, 12 figures, accepted for publication in A&A",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We study the abundance of star-forming and quiescent galaxies in a sample of 21 massive clusters at 0.5<z<0.7, detected with the Planck satellite. We measure the cluster galaxy stellar mass function (SMF), which is a fundamental observable to study and constrain the formation and evolution of galaxies. Our measurements are based on homogeneous and deep multi-band photometry spanning u- to the Ks-band for each cluster and are supported by spectroscopic data from different programs. The galaxy population is separated between quiescent and star-forming galaxies based on their rest-frame U-V and V-J colours. The SMF is compared to that of field galaxies at the same redshifts, using data from the COSMOS/UltraVISTA survey. We find that the shape of the SMF of star-forming galaxies does not depend on environment, while the SMF of quiescent galaxies has a significantly steeper low-mass slope in the clusters compared to the field. We estimate the environmental quenching efficiency (f_EQ), i.e. the probability for a galaxy that would normally be star forming in the field, to be quenched due to its environment. The f_EQ shows no stellar-mass dependence in any environment, but it increases from 40% in the cluster outskirts to ~90% in the cluster centres. The radial signature of f_EQ provides constraints on where the dominant quenching mechanism operates in these clusters and on what timescale. Exploring these using a simple model based on galaxy orbits obtained from an N-body simulation, we find a clear degeneracy between both parameters. For example, the quenching process may either be triggered on a long (~3 Gyr) time scale at large radii (r~8R_500), or happen well within 1 Gyr at r<R_500. The radius where quenching is triggered is at least r_quench> 0.67R_500 (95%CL). The ICM density at this location suggests that ram-pressure stripping of the cold gas is a likely cause of quenching. [Abridged]",
  "revisions": [
    {
      "version": "v1",
      "updated": "2018-07-02T18:00:00.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "stellar mass function",
      "planck-selected clusters",
      "satellite quenching",
      "constraints",
      "quiescent galaxies"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 16,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}