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Probing the galaxy-halo connection in UltraVISTA to z∼2

McCracken, H. J. ; Wolk, M. ; Colombi, S. ; Kilbinger, M. ; Ilbert, O. ; Peirani, S. ; Coupon, J. ; Dunlop, J. ; Milvang-Jensen, B. ; Caputi, K. ; Aussel, H. ; Béthermin, M. ; Le Fèvre, O.

In: Monthly Notices of the Royal Astronomical Society, 2015, vol. 449, no. 1, p. 901-916

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    Titre
    • Probing the galaxy-halo connection in UltraVISTA to z∼2
    Auteur
    • McCracken, H. J.. Sorbonne Universiteìs, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France
    • Wolk, M.. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France
    • Colombi, S.. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France
    • Kilbinger, M.. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France
    • Ilbert, O.. Laboratoire d'Astrophysique de Marseille, UMR 7326, 38 rue Frédéric Joliot-Curie, F-13388 Marseille cedex 13, France
    • Peirani, S.. Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France
    • Coupon, J.. Astronomical Observatory of the University of Geneva, ch. d'Ecogia 16, CH-1290 Versoix, Switzerland
    • Dunlop, J.. SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJL, UK
    • Milvang-Jensen, B.. Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
    • Caputi, K.. Kapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the Netherlands
    • Aussel, H.. CEA Saclay, Service d'Astrophysique (SAp), Orme des Merisiers, Bât. 709, F-91191 Gif-sur-Yvette, France
    • Béthermin, M.. European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
    • Le Fèvre, O.. Laboratoire d'Astrophysique de Marseille, UMR 7326, 38 rue Frédéric Joliot-Curie, F-13388 Marseille cedex 13, France
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2015, vol. 449, no. 1, p. 901-916. Oxford University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:290134
    Summary
    We use percent-level precision photometric redshifts in the UltraVISTA-DR1 near-infrared survey to investigate the changing relationship between galaxy stellar mass and the dark matter haloes hosting them to z∼2. We achieve this by measuring the clustering properties and abundances of a series of volume-limited galaxy samples selected by stellar mass and star formation activity. We interpret these results in the framework of a phenomenological halo model and numerical simulations. Our measurements span a uniquely large range in stellar mass and redshift and reach below the characteristic stellar mass to z∼2. Our results are: (1) at fixed redshift and scale, clustering amplitude depends monotonically on sample stellar mass threshold; (2) at fixed angular scale, the projected clustering amplitude decreases with redshift but the comoving correlation length remains constant; (3) characteristic halo masses and galaxy bias increase with increasing median stellar mass of the sample; (4) the slope of these relationships is modified in lower mass haloes; (5) concerning the passive galaxy population, characteristic halo masses are consistent with a simply less-abundant version of the full galaxy sample, but at lower redshifts the fraction of satellite galaxies in the passive population is very different from the full galaxy sample; (6) finally, we find that the ratio between the characteristic halo mass and median stellar mass at each redshift bin reaches a peak at log (Mh/M⊙)∼12.2 and the position of this peak remains constant out to z∼2. The behaviour of the full and passively evolving galaxy samples can be understood qualitatively by considering the slow evolution of the characteristic stellar mass in the redshift range probed by our survey