Evolution of clustering length, large-scale bias, and host halo mass at 2 < z < 5 in the VIMOS Ultra Deep Survey (VUDS)⋆
Journal
Date Issued
2015
Author(s)
Durkalec, A.
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Le Fèvre, O.
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Pollo, A.
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Cassata, P.
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Le Brun, V.
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Lemaux, B. C.
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Maccagni, D.
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Tasca, L. A. M.
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Thomas, R.
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Zamorani, G.
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Amorín, R.
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•
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Cimatti, A.
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•
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Giavalisco, M.
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Hathi, N. P.
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Ilbert, O.
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Paltani, S.
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Ribeiro, B.
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Schaerer, D.
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Sommariva, V.
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Talia, M.
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Tresse, L.
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Capak, P.
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Charlot, S.
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Contini, T.
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Cuby, J. G.
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Dunlop, J.
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Fotopoulou, S.
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Koekemoer, A.
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López-Sanjuan, C.
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Mellier, Y.
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Pforr, J.
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Salvato, M.
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Scoville, N.
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Taniguchi, Y.
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Wang, P. W.
Description
We thank Martin Kilbinger for assistance with implementing our HOD model into the CosmoPMC code. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010–2011. This work is based on data products made available at the CESAM data centre, Laboratoire d’Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This work is supported by the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02). A.P. is supported by the Polish National Science Centre grant UMO-2012/07/B/ST9/04425 and the Polish-Swiss Astro Project. Research conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant DEC-2013/08/M/ST9/00664.
Abstract
We investigate the evolution of galaxy clustering for galaxies in the redshift range 2.0 p(rp) measured by using 3022 galaxies with robust spectroscopic redshifts in two independent fields (COSMOS and VVDS-02h) covering in total 0.8deg2. We quantify how the scale dependent clustering amplitude r0 changes with redshift making use of mock samples to evaluate and correct the survey selection function. Using a power-law model ξ(r) = (r/r0)- γ we find that the correlation function for the general population is best fit by a model with a clustering length r0 = 3.95+0.48-0.54 h-1 Mpc and slope γ = 1.8+0.02-0.06 at z ~ 2.5, r0 = 4.35 ± 0.60 h-1 Mpc and γ = 1.6+0.12-0.13 at z ~ 3.5. We use these clustering parameters to derive the large-scale linear galaxy bias bLPL, between galaxies and dark matter. We find bLPL = 2.68 ± 0.22 at redshift z ~ 3 (assuming σ8 = 0.8), significantly higher than found at intermediate and low redshifts for the similarly general galaxy populations. We fit a halo occupation distribution (HOD) model to the data and we obtain that the average halo mass at redshift z ~ 3 is Mh = 1011.75 ± 0.23 h-1M☉. From this fit we confirm that the large-scale linear galaxy bias is relatively high at bLHOD = 2.82 ± 0.27. Comparing these measurements with similar measurements at lower redshifts we infer that the star-forming population of galaxies at z ~ 3 should evolve into the massive and bright (Mr< -21.5)galaxy population, which typically occupy haloes of mass ⟨ Mh ⟩ = 1013.9 h-1M☉ at redshift z = 0.
Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791.Appendices are available in electronic form at http://www.aanda.org
Volume
583
Start page
A128
Issn Identifier
0004-6361
Ads BibCode
2015A&A...583A.128D
Rights
open.access
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