Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey: I. The evolution of the mass-metallicity relation up to z ∼ 0.9

F. Lamareille, J. Brinchmann, T. Contini, C. J. Walcher, S. Charlot, E. Pérez-Montero, G. Zamorani, L. Pozzetti, M. Bolzonella, B. Garilli, S. Paltani, A. Bongiorno, O. Le Fèvre, D. Bottini, V. Le Brun, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. VettolaniA. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, A. Cappi, P. Ciliegi, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pellò, A. Pollo, M. Radovich, D. Vergani, E. Zucca, A. Romano, A. Grado, L. Limatola

Resultado de la investigación: Article

72 Citas (Scopus)

Resumen

Aims. We want to derive the mass-metallicity relation of star-forming galaxies up to z ∼ 0.9, using data from the VIMOS VLT Deep Survey. The mass-metallicity relation is commonly understood as the relation between the stellar mass and the gas-phase oxygen abundance.Methods. Automatic measurement of emission-line fluxes and equivalent widths have been performed on the full spectroscopic sample of the VIMOS VLT Deep Survey. This sample is divided into two sub-samples depending on the apparent magnitude selection: wide (I AB < 22.5) and deep (IAB < 24). These two samples span two different ranges of stellar masses. Emission-line galaxies have been separated into star-forming galaxies and active galactic nuclei using emission line ratios. For the star-forming galaxies the emission line ratios have also been used to estimate gas-phase oxygen abundance, using empirical calibrations renormalized in order to give consistent results at low and high redshifts. The stellar masses have been estimated by fitting the whole spectral energy distributions with a set of stellar population synthesis models.Results. We assume at first order that the shape of the mass-metallicity relation remains constant with redshift. Then we find a stronger metallicity evolution in the wide sample as compared to the deep sample. We thus conclude that the mass-metallicity relation is flatter at higher redshift. At z ∼ 0.77, galaxies at 109.4 solar masses have -0.18 dex lower metallicities than galaxies of similar masses in the local universe, while galaxies at 10 10.2 solar masses have -0.28 dex lower metallicities. By comparing the mass-metallicity and luminosity-metallicity relations, we also find an evolution in mass-to-light ratio: galaxies at higher redshifts being more active. The observed flattening of the mass-metallicity relation at high redshift is analyzed as evidence in favor of the open-closed model.

Idioma originalEnglish
Páginas (desde-hasta)53-72
Número de páginas20
PublicaciónAstronomy and Astrophysics
Volumen495
N.º1
DOI
EstadoPublished - 1 feb 2009

Huella dactilar

metallicity
physical property
physical properties
galaxies
stellar mass
stars
vapor phases
mass to light ratios
flattening
oxygen
spectral energy distribution
active galactic nuclei
universe
gas
luminosity
synthesis
estimates
calibration

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Lamareille, F. ; Brinchmann, J. ; Contini, T. ; Walcher, C. J. ; Charlot, S. ; Pérez-Montero, E. ; Zamorani, G. ; Pozzetti, L. ; Bolzonella, M. ; Garilli, B. ; Paltani, S. ; Bongiorno, A. ; Le Fèvre, O. ; Bottini, D. ; Le Brun, V. ; 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. ; Pellò, R. ; Pollo, A. ; Radovich, M. ; Vergani, D. ; Zucca, E. ; Romano, A. ; Grado, A. ; Limatola, L. / Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey : I. The evolution of the mass-metallicity relation up to z ∼ 0.9. En: Astronomy and Astrophysics. 2009 ; Vol. 495, N.º 1. pp. 53-72.
@article{b36d5c0107ff490a9de44fd5a72aead1,
title = "Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey: I. The evolution of the mass-metallicity relation up to z ∼ 0.9",
abstract = "Aims. We want to derive the mass-metallicity relation of star-forming galaxies up to z ∼ 0.9, using data from the VIMOS VLT Deep Survey. The mass-metallicity relation is commonly understood as the relation between the stellar mass and the gas-phase oxygen abundance.Methods. Automatic measurement of emission-line fluxes and equivalent widths have been performed on the full spectroscopic sample of the VIMOS VLT Deep Survey. This sample is divided into two sub-samples depending on the apparent magnitude selection: wide (I AB < 22.5) and deep (IAB < 24). These two samples span two different ranges of stellar masses. Emission-line galaxies have been separated into star-forming galaxies and active galactic nuclei using emission line ratios. For the star-forming galaxies the emission line ratios have also been used to estimate gas-phase oxygen abundance, using empirical calibrations renormalized in order to give consistent results at low and high redshifts. The stellar masses have been estimated by fitting the whole spectral energy distributions with a set of stellar population synthesis models.Results. We assume at first order that the shape of the mass-metallicity relation remains constant with redshift. Then we find a stronger metallicity evolution in the wide sample as compared to the deep sample. We thus conclude that the mass-metallicity relation is flatter at higher redshift. At z ∼ 0.77, galaxies at 109.4 solar masses have -0.18 dex lower metallicities than galaxies of similar masses in the local universe, while galaxies at 10 10.2 solar masses have -0.28 dex lower metallicities. By comparing the mass-metallicity and luminosity-metallicity relations, we also find an evolution in mass-to-light ratio: galaxies at higher redshifts being more active. The observed flattening of the mass-metallicity relation at high redshift is analyzed as evidence in favor of the open-closed model.",
keywords = "Galaxies: abundances, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: starburst",
author = "F. Lamareille and J. Brinchmann and T. Contini and Walcher, {C. J.} and S. Charlot and E. P{\'e}rez-Montero and G. Zamorani and L. Pozzetti and M. Bolzonella and B. Garilli and S. Paltani and A. Bongiorno and {Le F{\`e}vre}, O. and D. Bottini and {Le Brun}, V. and D. Maccagni and R. Scaramella and M. Scodeggio and L. Tresse and G. Vettolani and A. Zanichelli and C. Adami and S. Arnouts and S. Bardelli and A. Cappi and P. Ciliegi and S. Foucaud and P. Franzetti and I. Gavignaud and L. Guzzo and O. Ilbert and A. Iovino and McCracken, {H. J.} and B. Marano and C. Marinoni and A. Mazure and B. Meneux and R. Merighi and R. Pell{\`o} and A. Pollo and M. Radovich and D. Vergani and E. Zucca and A. Romano and A. Grado and L. Limatola",
year = "2009",
month = "2",
day = "1",
doi = "10.1051/0004-6361:200810397",
language = "English",
volume = "495",
pages = "53--72",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
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Lamareille, F, Brinchmann, J, Contini, T, Walcher, CJ, Charlot, S, Pérez-Montero, E, Zamorani, G, Pozzetti, L, Bolzonella, M, Garilli, B, Paltani, S, Bongiorno, A, Le Fèvre, O, Bottini, D, Le Brun, V, 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, HJ, Marano, B, Marinoni, C, Mazure, A, Meneux, B, Merighi, R, Pellò, R, Pollo, A, Radovich, M, Vergani, D, Zucca, E, Romano, A, Grado, A & Limatola, L 2009, 'Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey: I. The evolution of the mass-metallicity relation up to z ∼ 0.9', Astronomy and Astrophysics, vol. 495, n.º 1, pp. 53-72. https://doi.org/10.1051/0004-6361:200810397

Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey : I. The evolution of the mass-metallicity relation up to z ∼ 0.9. / Lamareille, F.; Brinchmann, J.; Contini, T.; Walcher, C. J.; Charlot, S.; Pérez-Montero, E.; Zamorani, G.; Pozzetti, L.; Bolzonella, M.; Garilli, B.; Paltani, S.; Bongiorno, A.; Le Fèvre, O.; Bottini, D.; Le Brun, V.; 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.; Pellò, R.; Pollo, A.; Radovich, M.; Vergani, D.; Zucca, E.; Romano, A.; Grado, A.; Limatola, L.

En: Astronomy and Astrophysics, Vol. 495, N.º 1, 01.02.2009, p. 53-72.

Resultado de la investigación: Article

TY - JOUR

T1 - Physical properties of galaxies and their evolution in the VIMOS VLT Deep Survey

T2 - I. The evolution of the mass-metallicity relation up to z ∼ 0.9

AU - Lamareille, F.

AU - Brinchmann, J.

AU - Contini, T.

AU - Walcher, C. J.

AU - Charlot, S.

AU - Pérez-Montero, E.

AU - Zamorani, G.

AU - Pozzetti, L.

AU - Bolzonella, M.

AU - Garilli, B.

AU - Paltani, S.

AU - Bongiorno, A.

AU - Le Fèvre, O.

AU - Bottini, D.

AU - Le Brun, V.

AU - Maccagni, D.

AU - Scaramella, R.

AU - Scodeggio, M.

AU - Tresse, L.

AU - Vettolani, G.

AU - Zanichelli, A.

AU - Adami, C.

AU - Arnouts, S.

AU - Bardelli, S.

AU - Cappi, A.

AU - Ciliegi, P.

AU - Foucaud, S.

AU - Franzetti, P.

AU - Gavignaud, I.

AU - Guzzo, L.

AU - Ilbert, O.

AU - Iovino, A.

AU - McCracken, H. J.

AU - Marano, B.

AU - Marinoni, C.

AU - Mazure, A.

AU - Meneux, B.

AU - Merighi, R.

AU - Pellò, R.

AU - Pollo, A.

AU - Radovich, M.

AU - Vergani, D.

AU - Zucca, E.

AU - Romano, A.

AU - Grado, A.

AU - Limatola, L.

PY - 2009/2/1

Y1 - 2009/2/1

N2 - Aims. We want to derive the mass-metallicity relation of star-forming galaxies up to z ∼ 0.9, using data from the VIMOS VLT Deep Survey. The mass-metallicity relation is commonly understood as the relation between the stellar mass and the gas-phase oxygen abundance.Methods. Automatic measurement of emission-line fluxes and equivalent widths have been performed on the full spectroscopic sample of the VIMOS VLT Deep Survey. This sample is divided into two sub-samples depending on the apparent magnitude selection: wide (I AB < 22.5) and deep (IAB < 24). These two samples span two different ranges of stellar masses. Emission-line galaxies have been separated into star-forming galaxies and active galactic nuclei using emission line ratios. For the star-forming galaxies the emission line ratios have also been used to estimate gas-phase oxygen abundance, using empirical calibrations renormalized in order to give consistent results at low and high redshifts. The stellar masses have been estimated by fitting the whole spectral energy distributions with a set of stellar population synthesis models.Results. We assume at first order that the shape of the mass-metallicity relation remains constant with redshift. Then we find a stronger metallicity evolution in the wide sample as compared to the deep sample. We thus conclude that the mass-metallicity relation is flatter at higher redshift. At z ∼ 0.77, galaxies at 109.4 solar masses have -0.18 dex lower metallicities than galaxies of similar masses in the local universe, while galaxies at 10 10.2 solar masses have -0.28 dex lower metallicities. By comparing the mass-metallicity and luminosity-metallicity relations, we also find an evolution in mass-to-light ratio: galaxies at higher redshifts being more active. The observed flattening of the mass-metallicity relation at high redshift is analyzed as evidence in favor of the open-closed model.

AB - Aims. We want to derive the mass-metallicity relation of star-forming galaxies up to z ∼ 0.9, using data from the VIMOS VLT Deep Survey. The mass-metallicity relation is commonly understood as the relation between the stellar mass and the gas-phase oxygen abundance.Methods. Automatic measurement of emission-line fluxes and equivalent widths have been performed on the full spectroscopic sample of the VIMOS VLT Deep Survey. This sample is divided into two sub-samples depending on the apparent magnitude selection: wide (I AB < 22.5) and deep (IAB < 24). These two samples span two different ranges of stellar masses. Emission-line galaxies have been separated into star-forming galaxies and active galactic nuclei using emission line ratios. For the star-forming galaxies the emission line ratios have also been used to estimate gas-phase oxygen abundance, using empirical calibrations renormalized in order to give consistent results at low and high redshifts. The stellar masses have been estimated by fitting the whole spectral energy distributions with a set of stellar population synthesis models.Results. We assume at first order that the shape of the mass-metallicity relation remains constant with redshift. Then we find a stronger metallicity evolution in the wide sample as compared to the deep sample. We thus conclude that the mass-metallicity relation is flatter at higher redshift. At z ∼ 0.77, galaxies at 109.4 solar masses have -0.18 dex lower metallicities than galaxies of similar masses in the local universe, while galaxies at 10 10.2 solar masses have -0.28 dex lower metallicities. By comparing the mass-metallicity and luminosity-metallicity relations, we also find an evolution in mass-to-light ratio: galaxies at higher redshifts being more active. The observed flattening of the mass-metallicity relation at high redshift is analyzed as evidence in favor of the open-closed model.

KW - Galaxies: abundances

KW - Galaxies: evolution

KW - Galaxies: fundamental parameters

KW - Galaxies: starburst

UR - http://www.scopus.com/inward/record.url?scp=60849136363&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:200810397

DO - 10.1051/0004-6361:200810397

M3 - Article

AN - SCOPUS:60849136363

VL - 495

SP - 53

EP - 72

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 1

ER -