Volume 520, September-October 2010
|Number of page(s)||20|
|Section||Catalogs and data|
|Published online||29 September 2010|
The VIMOS-VLT deep survey: the group catalogue*
INAF-Osservatorio Astronomico di Brera, via Brera 28, 20021 Milan, Italy e-mail: firstname.lastname@example.org
2 Laboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, 38 rue Frederic Joliot-Curie, 13388 Marseille Cedex 13, France
3 Centre de Physique Théorique, UMR 6207, CNRS-Université de Provence, 13288 Marseille, France
4 INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
5 IASF-INAF, via Bassini 15, 20133 Milano, Italy
6 Institute of Astro- and Particle Physics, Leopold-Franzens-University Innsbruck, Technikerstraße 25, 6020 Innsbruck, Austria
7 INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy
8 Université de Lyon, 69003 Lyon, France; Université Lyon 1, Observatoire de Lyon, 9 avenue Charles André, Saint-Genis Laval, 69230, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon; École Normale Supérieure de Lyon, 69007 Lyon, France
9 Max Planck Institut für Extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching bei München, Germany
10 Universitätssternwarte München, Scheinerstrasse 1, 81679 München, Germany
11 IRA-INAF, via Gobetti 101, 40129 Bologna, Italy
12 Canada France Hawaii Telescope corporation, Mamalahoa Hwy, Kamuela, 96743, USA
13 Max Planck Institut für Astrophysik, 85741 Garching, Germany
14 Institut d'Astrophysique de Paris, UMR 7095, 98 bis Bvd Arago, 75014 Paris, France
15 Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, 14 Av. E. Belin, 31400 Toulouse, France
16 School of Physics & Astronomy, University of Nottingham, University Park, Nottingham, NG72RD, UK
17 Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
18 Observatoire de Paris, LERMA, 61 Avenue de l'Observatoire, 75014 Paris, France
19 Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy
20 Integral Science Data Centre, ch. d'Écogia 16, 1290 Versoix, Switzerland
21 Geneva Observatory, ch. des Maillettes 51, 1290 Sauverny, Switzerland
22 The Andrzej Soltan Institute for Nuclear Studies, ul. Hoza 69, 00-681 Warszawa, Poland
23 Astronomical Observatory of the Jagiellonian University, ul Orla 171, 30-244 Kraków, Poland
24 Instituto de Astrofísica de Andalucía – CSIC. Apdo. de correos 3004, 18080 Granada, Spain
Accepted: 7 May 2010
Aims. We present a homogeneous and complete catalogue of optical galaxy groups identified in the purely flux-limited (17.5 ≤ IAB ≤ 24.0) VIMOS-VLT deep redshift Survey (VVDS).
Methods. We use mock catalogues extracted from the Millennium Simulation, to correct for potential systematics that might affect the overall distribution as well as the individual properties of the identified systems. Simulated samples allow us to forecast the number and properties of groups that can be potentially found in a survey with VVDS-like selection functions. We use them to correct for the expected incompleteness and, to asses in addition, how well galaxy redshifts trace the line-of-sight velocity dispersion of the underlying mass overdensity. In particular, on these mock catalogues we train the adopted group-finding technique i.e., the Voronoi-Delaunay Method (VDM). The goal is to fine-tune its free parameters, recover in a robust and unbiased way the redshift and velocity dispersion distributions of groups (n(z) and n(σ), respectively), and maximize, at the same time, the level of completeness and purity of the group catalogue.
Results. We identify 318 VVDS groups with at least 2 members in the range 0.2 ≤ z ≤ 1.0, among which 144 (/30) with at least 3 (/5) members. The sample has an overall completeness of ~60% and a purity of ~50%. Nearly 45% of the groups with at least 3 members are still recovered if we run the algorithm with a particular parameter set that maximizes the purity (~75%) of the resulting catalogue. We use the group sample to explore the redshift evolution of the fraction fb of blue galaxies (U–B ≤ 1) in the redshift range 0.2 ≤ z ≤ 1. We find that the fraction of blue galaxies is significantly lower in groups than in the global population (i.e. in the whole ensemble of galaxies irrespective of their environment). Both of these quantities increase with redshift, the fraction of blue galaxies in groups exhibiting a marginally significant steeper increase. We also investigate the dependence of fb on group richness: not only we confirm that, at any redshift, the blue fraction decreases in systems with increasing richness, but we find that this result continues to hold towards fainter luminosities.
Key words: galaxies: clusters: general / large-scale structure of Universe / galaxies: high-redshift / galaxies: evolution / galaxies: statistics
Complete Tables 4 and 5 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/520/A42
© ESO, 2010
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.