2009A&A...495...73P


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.18CEST08:07:45

2009A&A...495...73P - Astronomy and Astrophysics, volume 495, 73-81 (2009/2-3)

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.

PEREZ-MONTERO E., CONTINI T., LAMAREILLE F., BRINCHMANN J., WALCHER C.J., CHARLOT S., BOLZONELLA M., POZZETTI L., BOTTINI D., GARILLI B., LE BRUN V., LE FEVRE O., MACCAGNI D., SCARAMELLA R., SCODEGGIO M., TRESSE L., VETTOLANI G., ZANICHELLI A., ADAMI C., ARNOUTS S., BARDELLI S., CAPPI A., CILIEGI P., FOUCAUD S., FRANZETTI P., GAVIGNAUD I., GUZZO L., ILBERT O., IOVINO A., McCRACKEN H.J., MARANO B., MARINONI C., MAZURE A., MENEUX B., MERIGHI R., PALTANI S., PELLO R., POLLO A., RADOVICH M., VERGANI D., ZAMORANI G. and ZUCCA E.

Abstract (from CDS):

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. 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. 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 ∼0.3dex lower than galaxies in the local universe. However we do not see any significant metallicity evolution between redshifts z∼0.7 (Paper I, Lamareille et al., 2009A&A...495...53L) 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.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: fundamental parameters - galaxies: abundances - galaxies: starburst

Simbad objects: 24

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Number of rows : 24

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 VIDEO J022503.27-044729.44 G 02 25 03.25 -04 47 29.2   23.743 23.577 23.531 23.126 ~ 6 0
2 VIDEO J022506.64-043328.25 GiP 02 25 06.64 -04 33 27.9   23.281 23.171 23.096 22.616 ~ 7 0
3 VIDEO J022547.12-042107.79 G 02 25 47.139 -04 21 07.60   23.889 23.738 23.625 22.801 ~ 12 0
4 VIDEO J022547.65-043807.81 G 02 25 47.678 -04 38 07.62   24.019 23.874 23.610 23.108 ~ 7 0
5 VIDEO J022549.66-040912.00 G 02 25 49.68 -04 09 11.9   22.449 22.236 22.054 21.429 ~ 6 0
6 VIDEO J022553.89-042337.25 G 02 25 53.92 -04 23 36.9   23.128 22.672 22.397 21.712 ~ 6 0
7 VIDEO J022556.03-043646.25 G 02 25 56.04 -04 36 46.0   23.772 23.545 23.431 23.181 ~ 6 0
8 VVDS 020210745 G 02 26 04.08 -04 31 50.8   25.508 24.793 25.280 23.967 ~ 5 0
9 VIDEO J022605.25-044136.04 G 02 26 05.263 -04 41 36.06   23.055 22.735 22.664 22.156 ~ 7 0
10 VIDEO J022611.19-044329.24 G 02 26 11.187 -04 43 28.94   24.494 23.562 23.101 22.360 ~ 5 0
11 VIDEO J022612.29-041721.65 G 02 26 12.30 -04 17 21.6   24.116 23.946 23.667 22.889 ~ 6 0
12 VIDEO J022639.60-042413.39 G 02 26 39.61 -04 24 13.1   24.060 23.938 23.797 23.357 ~ 6 0
13 VIDEO J022643.18-044014.51 G 02 26 43.223 -04 40 14.25   23.977 23.798 23.820 23.193 ~ 7 0
14 VIDEO J022646.42-042722.37 G 02 26 46.430 -04 27 21.97   24.212 24.332 23.551 23.371 ~ 5 0
15 VIDEO J022701.71-043310.94 G 02 27 01.73 -04 33 10.8   23.677 23.585 23.636 23.268 ~ 6 0
16 VIDEO J022710.75-044556.38 G 02 27 10.760 -04 45 56.43   23.172 22.988 22.975 22.499 ~ 7 0
17 VIDEO J022711.84-040836.32 G 02 27 11.86 -04 08 36.1   24.695 24.456 24.058 23.764 ~ 6 0
18 VIDEO J022712.24-042311.33 G 02 27 12.256 -04 23 11.22   23.947 23.747 23.703 23.446 ~ 11 0
19 VIDEO J022713.43-042231.82 G 02 27 13.45 -04 22 31.8   23.482 23.377 23.355 22.758 ~ 6 0
20 VIDEO J022713.97-040859.78 G 02 27 13.988 -04 08 59.56   23.326 23.120 23.111 22.582 ~ 13 0
21 VIDEO J022735.21-043348.16 G 02 27 35.22 -04 33 48.0   23.858 23.575 23.670 23.119 ~ 6 0
22 VIDEO J022749.39-043943.79 G 02 27 49.392 -04 39 43.77   22.995 22.853 22.703 22.174 ~ 7 0
23 VIDEO J022809.51-041945.94 G 02 28 09.52 -04 19 45.8   24.807 24.548 24.148 23.455 ~ 6 0
24 NAME Chandra Deep Field-South reg 03 32 28.0 -27 48 30           ~ 1878 1

    Equat.    Gal    SGal    Ecl

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2021.05.18-08:07:45

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