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Aims. We present a continuation of our study about the relation betweenstellar mass and gas-phase metallicity in the VIMOS VLT Deep Survey (VVDS). Inthis work we extend the determination of metallicities up to redshift = 1.24for 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 bothdiagnostic diagrams and empirical calibrations based on [OII] emission linesalong with the empirical relation between the intensities of the [OIII] and[NeIII] emission lines and the theoretical ratios between Balmer recombinationemission lines to identify star-forming galaxies and to derive theirmetallicities. We derive stellar masses by fitting the whole spectral energydistribution with a set of stellar population synthesis models. Results. Thesenew methods allow us to extend the mass-metallicity relation to higherredshift. We show that the metallicity determinations are consistent with moreestablished strong-line methods. Taken together this allows us to study theevolution of the mass-metallicity relation up to z = 1.24 with good control ofsystematic uncertainties. We find an evolution with redshift of the averagemetallicity of galaxies very similar to those reported in the literature: for agiven stellar mass, galaxies at z = 1 have, on average, a metallicity = 0.3 dexlower than galaxies in the local universe. However we do not see anysignificant metallicity evolution between redshifts z = 0.7 (Paper I) and z =1.0 (this paper). We find also the same flattening of the mass-metallicityrelation for the most massive galaxies as reported in Paper I at lowerredshifts, but again no apparent evolution of the slope is seen between z = 0.7and z = 1.0.

astronomy and astrophysics

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