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Title:
VVDS-SWIRE. Clustering evolution from a spectroscopic sample of galaxies with redshift 0.2 < z < 2.1 selected from Spitzer IRAC 3.6 μ m and 4.5 μ m photometry
Authors:
de la Torre, S.; Le Fèvre, O.; Arnouts, S.; Guzzo, L.; Farrah, D.; Iovino, A.; Lonsdale, C. J.; Meneux, B.; Oliver, S. J.; Pollo, A.; Waddington, I.; Bottini, D.; Fang, F.; Garilli, B.; Le Brun, V.; Maccagni, D.; Picat, J. P.; Scaramella, R.; Scodeggio, M.; Shupe, D.; Surace, J.; Tresse, L.; Vettolani, G.; Zanichelli, A.; Adami, C.; Bardelli, S.; Bolzonella, M.; Cappi, A.; Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Ilbert, O.; Lamareille, F.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure, A.; Merighi, R.; Paltani, S.; Pellò, R.; Pozzetti, L.; Radovich, M.; Zamorani, G.; Zucca, E.; Bondi, M.; Bongiorno, A.; Brinchmann, J.; Cucciati, O.; Mellier, Y.; Merluzzi, P.; Temporin, S.; Vergani, D.; Walcher, C. J.
Affiliation:
AA(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France ), AB(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AC(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AD(INAF-Osservatorio Astronomico di Brera, via Brera 28, Milan, Italy), AE(Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA), AF(INAF-Osservatorio Astronomico di Brera, via Brera 28, Milan, Italy), AG(Infrared Processing & Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USA ; Center for Astrophysics & Space Sciences, University of California San Diego, La Jolla, CA 92093-0424, USA), AH(INAF-Osservatorio Astronomico di Brera, via Brera 28, Milan, Italy ; IASF-INAF, via Bassini 15, 20133 Milano, Italy), AI(Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK), AJ(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France; Geneva Observatory, ch. des Maillettes 51, 1290 Sauverny, Switzerland), AK(Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK), AL(IASF-INAF, via Bassini 15, 20133 Milano, Italy), AM(Spitzer Science Center, California Institute of Technology, Mail Stop 314-6, 1200 East California Boulevard, Pasadena, CA 91125, USA), AN(IASF-INAF, via Bassini 15, 20133 Milano, Italy), AO(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AP(IASF-INAF, via Bassini 15, 20133 Milano, Italy), AQ(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), 14 avenue E. Belin, 31400 Toulouse, France), AR(IRA-INAF, via Gobetti, 101, 40129 Bologna, Italy ; INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), AS(IASF-INAF, via Bassini 15, 20133 Milano, Italy), AT(Infrared Processing & Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USA), AU(Spitzer Science Center, California Institute of Technology, Mail Stop 314-6, 1200 East California Boulevard, Pasadena, CA 91125, USA), AV(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AW(IRA-INAF, via Gobetti, 101, 40129 Bologna, Italy), AX(IRA-INAF, via Gobetti, 101, 40129 Bologna, Italy), AY(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AZ(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BA(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BB(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BC(Max Planck Institut fur Astrophysik, 85741, Garching, Germany ; Institut d'Astrophysique de Paris, UMR 7095, 98bis Bvd. Arago, 75014 Paris, France), BD(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BE(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), 14 avenue E. Belin, 31400 Toulouse, France), BF(School of Physics & Astronomy, University of Nottingham, University Park, Nottingham, NG72RD, UK), BG(IASF-INAF, via Bassini 15, 20133 Milano, Italy), BH(Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany), BI(Institute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, 96822, Hawaii), BJ(Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy), BK(Institut d'Astrophysique de Paris, UMR 7095, 98bis Bvd. Arago, 75014 Paris, France ; Observatoire de Paris, LERMA, 61 avenue de l'Observatoire, 75014 Paris, France), BL(Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy), BM(Centre de Physique Théorique, UMR 6207 CNRS-Université de Provence, 13288 Marseille, France), BN(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), BO(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BP(Integral Science Data Centre, Ch. d'Écogia 16, 1290 Versoix, Switzerland ; Geneva Observatory, ch. des Maillettes 51, 1290 Sauverny, Switzerland), BQ(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), 14 avenue E. Belin, 31400 Toulouse, France), BR(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BS(INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy), BT(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BU(INAF-Osservatorio Astronomico di Bologna, via Ranzani, 1, 40127 Bologna, Italy), BV(IRA-INAF, via Gobetti, 101, 40129 Bologna, Italy), BW(Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy), BX(Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal), BY(INAF-Osservatorio Astronomico di Brera, via Brera 28, Milan, Italy ; Universitá di Milano-Bicocca, Dipartimento di Fisica, Piazza delle Scienze 3, 20126 Milano, Italy), BZ(Institut d'Astrophysique de Paris, UMR 7095, 98bis Bvd. Arago, 75014 Paris, France ; Observatoire de Paris, LERMA, 61 avenue de l'Observatoire, 75014 Paris, France), CA(INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy), CB(INAF-Osservatorio Astronomico di Brera, via Brera 28, Milan, Italy), CC(IASF-INAF, via Bassini 15, 20133 Milano, Italy), CD(Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France)
Publication:
Astronomy and Astrophysics, Volume 475, Issue 2, November IV 2007, pp.443-451 (A&A Homepage)
Publication Date:
11/2007
Origin:
EDP Sciences
Keywords:
cosmology: observations, cosmology: large-scale structure of, Universe, galaxies: evolution, galaxies: high-redshift, galaxies:, statistics, infrared: galaxies
DOI:
10.1051/0004-6361:20077161
Bibliographic Code:
2007A&A...475..443D

Abstract

Aims:By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m3.6)_AB < 21.5 at 3.6 μ m, and 1255 spectroscopic redshifts of galaxies with (m4.5)_AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1.
Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 μ m and 4.5 μ m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field.
Results: We find that in the 3.6 μ m and 4.5 μ m flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ≃ 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 μ m and a mean value of r0 ≃ 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 μ m, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24, for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 μm selected samples decreases with increasing redshift, becoming comparable at z ≃ 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ≃ 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.

Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, program 070.A-9007(A), and on data obtained at the Canada-France-Hawaii Telescope, operated by the CNRS of France, CNRC in Canada and the University of Hawaii, and 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 Science 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.

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