The VIMOS-VLT Deep Survey

A. Pollo; L. Guzzo; O. Le Fèvre; B. Meneux; A. Cappi; P. Franzetti; A. Iovino; H. J. McCracken; C. Marinoni; G. Zamorani; D. Bottini; B. Garilli; V. Le Brun; D. Maccagni; J. P. Picat; R. Scaramella; M. Scodeggio; L. Tresse; G. Vettolani; A. Zanichelli; C. Adami; S. Arnouts; S. Bardelli; M. Bolzonella; S. Charlot; P. Ciliegi; T. Contini; S. Foucaud; I. Gavignaud; O. Ilbert; B. Marano; A. Mazure; R. Merighi; S. Paltani; R. Pellò; L. Pozzetti; M. Radovich; E. Zucca; M. Bondi; A. Bongiorno; G. Busarello; O. Cucciati; L. Gregorini; F. Lamareille; G. Mathez; Y. Mellier; P. Merluzzi; V. Ripepi; D. Rizzo

doi:10.1051/0004-6361:20054705

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Volume 451 / No 2 (May IV 2006)

A&A, 451 2 (2006) 409-416

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Issue		A&A Volume 451, Number 2, May IV 2006


Page(s)		409 - 416
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361:20054705
Published online		02 May 2006

A&A 451, 409-416 (2006)

Luminosity dependence of clustering at z $\simeq 1$

A. Pollo¹^,2^,3, L. Guzzo², O. Le Fèvre¹, B. Meneux¹, A. Cappi⁴, P. Franzetti⁵, A. Iovino², H. J. McCracken⁶^,7, C. Marinoni⁸^,1, G. Zamorani⁴, D. Bottini⁵, B. Garilli⁵, V. Le Brun¹, D. Maccagni⁵, J. P. Picat⁹, R. Scaramella¹⁰, M. Scodeggio⁵, L. Tresse¹, G. Vettolani¹¹, A. Zanichelli¹¹, C. Adami¹, S. Arnouts¹, S. Bardelli⁴, M. Bolzonella¹², S. Charlot⁶, P. Ciliegi⁴, T. Contini⁹, S. Foucaud¹³, I. Gavignaud⁹^,14, O. Ilbert¹², B. Marano¹², A. Mazure¹, R. Merighi⁴, S. Paltani¹⁵^,16, R. Pellò⁹, L. Pozzetti⁴, M. Radovich¹⁷, E. Zucca⁴, M. Bondi¹¹, A. Bongiorno¹², G. Busarello¹⁷, O. Cucciati²^,18, L. Gregorini¹¹, F. Lamareille⁹, G. Mathez⁹, Y. Mellier⁶^,7, P. Merluzzi¹⁷, V. Ripepi¹⁷ and D. Rizzo¹⁹

¹ Laboratoire d'Astropysique de Marseile, UMR 6110 CNRS, Université de Provence, BP 8, 13376 Marseille Cedex 12, France e-mail: agnieszka.pollo@oamp.fr
² INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807, Merate & via Brera 28, 20121 Milano, Italy
³ Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland
⁴ INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
⁵ INAF – IASF Milano, via Bassini 15, 20133 Milano, Italy
⁶ Institut d'Astrophysique de Paris, UMR 7095, 98 bis Bvd Arago, 75014 Paris, France
⁷ Observatoire de Paris, LERMA, 61 Avenue de l'Observatoire, 75014 Paris, France
⁸ Centre de Physique Théorique CNRS – Luminy and Université de Provence, UMR 6207, 13288 Marseille Cedex 9, France
⁹ Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), 14 avenue E. Belin, 31400 Toulouse, France
¹⁰ INAF – Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy
¹¹ INAF – IRA, via Gobetti 101, 40129 Bologna, Italy
¹² Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy
¹³ School of Physics & Astronomy, University of Nottingham, University Park, Nottingham, NG72RD, UK
¹⁴ Universitat Postdam, Astrophysik, 14469 Postdam, Germany
¹⁵ Integral Science Data Centre, ch. d'Écogia 16, 1290 Versoix, Switzerland
¹⁶ Geneva Observatory, ch. des Maillettes 51, 1290 Sauverny, Switherland
¹⁷ INAF – Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
¹⁸ Universitá di Milano-Bicocca, Dipartimento di Fisica, Piazza delle Scienze 3, 20126 Milano, Italy
¹⁹ Imperial College London, South Kensington Campus, London SW7 2AZ, UK

Received: 16 December 2005
Accepted: 16 January 2006

Abstract

We investigate the dependence of galaxy clustering on the galaxy intrinsic luminosity at high redshift, using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). The size (6530 galaxies) and depth ( $I_{AB}<24$ ) of the survey allows us to measure the projected two-point correlation function of galaxies, $w_{\rm p}(r_{\rm p})$ , for a set of volume-limited samples up to an effective redshift $\left<z\right>=0.9$ and median absolute magnitude $-19.6< M_B < -21.3$ . Fitting $w_{\rm p}(r_{\rm p})$ with a single power-law model for the real-space correlation function $\xi(r)=(r/r_0)^{-\gamma}$ , we measure the relationship of the correlation length r₀ and the slope γ with the sample median luminosity for the first time at such high redshift. Values from our lower-redshift samples ( $0.1<z<0.5$ ) are fully consistent with the trend observed by larger local surveys. In our high redshift sample ( $0.5<z<1.2$ ), we find that the clustering strength suddenly rises around $M_B^*$ , apparently with a sharper inflection than at low redshifts. Galaxies in the faintest sample ( $\left<M_B\right>=-19.6$ ) have a correlation length $r_0=2.7^{+0.3}_{-0.3}$ h^-1 Mpc, compared to $r_0=5.0^{+1.5}_{-1.6}$ h^-1 Mpc at $\left<M_B\right>=-21.3$ . The slope of the correlation function is observed to correspondingly steepen significantly from $\gamma=1.6^{+0.1}_{-0.1}$ to $\gamma=2.4^{+0.4}_{-0.2}$ . This is not observed either by large local surveys or in our lower-redshift samples and seems to imply a significant change in the way luminous galaxies trace dark-matter halos at $z\sim 1$ with respect to $z\sim 0$ . At our effective median redshift $z \simeq 0.9$ this corresponds to a strong difference of the relative bias, from $b/b* < 0.7$ for galaxies with $L < L*$ to $b/b* \simeq 1.4$ for galaxies with $L > L*$ .  

Key words: cosmology: large scale structure of Universe / cosmology: observations / methods: statistical / galaxies: evolution

© ESO, 2006

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