Volume 495, Number 1, February III 2009
|Page(s)||73 - 81|
|Published online||15 October 2008|
Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey*
II. Extending the mass-metallicity relation to the range z ≈ 0.89–1.24
Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, Observatoire Midi-Pyrénées, 14 Av. E. Belin, 31400, Toulouse, France e-mail: firstname.lastname@example.org
2 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal
3 Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, 38 rue Frederic Joliot-Curie, 13388 Marseille Cedex 13, France
4 Max Planck Institut für Astrophysik, 85741, Garching, Germany
5 Institut d'Astrophysique de Paris, UMR 7095, 98 bis Bvd Arago, 75014, Paris, France
6 INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy
7 IASF-INAF, via Bassini 15, 20133, Milano, Italy
8 IRA-INAF, via Gobetti 101, 40129, Bologna, Italy
9 INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040, Monte Porzio Catone, Italy
10 Canada France Hawaii Telescope corporation, Mamalahoa Hwy, Kamuela, 96743, USA
11 School of Physics & Astronomy, University of Nottingham, University Park, Nottingham, NG72RD, UK
12 Astrophysical Institute Potsdam, An der Sternwarte 16, 14482, Potsdam, Germany
13 INAF-Osservatorio Astronomico di Brera, via Brera 28, 20021, Milan, Italy
14 Institute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, Hawaii, 96822, USA
15 Observatoire de Paris, LERMA, 61 Avenue de l'Observatoire, 75014, Paris, France
16 Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127, Bologna, Italy
17 Centre de Physique Théorique, UMR 6207 CNRS-Université de Provence, 13288, Marseille, France
18 Integral Science Data Centre, ch. d'Écogia 16, 1290, Versoix, Switzerland
19 Geneva Observatory, ch. des Maillettes 51, 1290, Sauverny, Switzerland
20 Astronomical Observatory of the Jagiellonian University, ul Orla 171, PL-30-244, Kraków, Poland
21 INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131, Napoli, Italy
Accepted: 3 October 2008
Aims. We present a continuation of our study about the relation between stellar mass and gas-phase metallicity in the VIMOS VLT Deep Survey (VVDS). In this work we extend the determination of metallicities up to redshift ≈1.24 for a sample of 42 star-forming galaxies with a mean redshift value of 0.99.
Methods. For a selected sample of emission-line galaxies, we use both diagnostic diagrams and empirical calibrations based on [Oii] emission lines along with the empirical relation between the intensities of the [Oiii] and [Neiii] emission lines and the theoretical ratios between Balmer recombination emission lines to identify star-forming galaxies and to derive their metallicities. We derive stellar masses by fitting the whole spectral energy distribution with a set of stellar population synthesis models.
Results. These new methods allow us to extend the mass-metallicity relation to higher redshift. We show that the metallicity determinations are consistent with more established strong-line methods. Taken together this allows us to study the evolution of the mass-metallicity relation up to z ≈ 1.24 with good control of systematic uncertainties. We find an evolution with redshift of the average metallicity of galaxies very similar to those reported in the literature: for a given stellar mass, galaxies at z ~ 1 have, on average, a metallicity ~ 0.3 dex lower than galaxies in the local universe. However we do not see any significant metallicity evolution between redshifts z ~ 0.7 (Paper I) and z ~ 1.0 (this paper). We find also the same flattening of the mass-metallicity relation for the most massive galaxies as reported in Paper I at lower redshifts, but again no apparent evolution of the slope is seen between z ~ 0.7 and z ~ 1.0.
Key words: galaxies: evolution / galaxies: fundamental parameters / galaxies: abundances / galaxies: starburst
© ESO, 2009
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