Mass-metallicity relation explored with CALIFA. I. Is there a dependence on the star-formation rate?
- Author(s)
- , S. F. Sánchez, Fabiàn Fabían Rosales-Ortega, Bruno Jungwiert, Jorge I. Iglesias-Páramo, J. M. Vílchez, Rosamaria A. Marino, Carl Jakob Walcher, B. Husemann, D. Mast, A. Monreal-Ibero, R. Cid Fernandes, E. Pérez, R. González Delgado, R. García-Benito, L. Galbany, G. van de Ven, K. Jahnke, H. Flores, J. Bland-Hawthorn, A. R. López-Sánchez, V. Stanishev, D. Miralles-Caballero, A. I. Díaz, P. Sánchez-Blazquez, M. Mollá, A. Gallazzi, P. Papaderos, J. M. Gomes, N. Gruel, I. Pérez, T. Ruiz-Lara, E. Florido, A. de Lorenzo-Cáceres, J. Mendez-Abreu, C. Kehrig, M. M. Roth, B. Ziegler, J. Alves, L. Wisotzki, D. Kupko, A. Quirrenbach, D. Bomans
- Abstract
We studied the global and local M-Z relation based on the first data
available from the CALIFA survey (150 galaxies). This survey provides
integral field spectroscopy of the complete optical extent of each
galaxy (up to 2-3 effective radii), with a resolution high enough to
separate individual H II regions and/or aggregations. About 3000
individual HII regions have been detected. The spectra cover the
wavelength range between [OII]3727 and [SII]6731, with a sufficient
signal-to-noise ratio to derive the oxygen abundance and star-formation
rate associated with each region. In addition, we computed the
integrated and spatially resolved stellar masses (and surface densities)
based on SDSS photometric data. We explore the relations between the
stellar mass, oxygen abundance and star-formation rate using this
dataset.
We derive a tight relation between the integrated stellar mass and the
gas-phase abundance, with a dispersion lower than the one already
reported in the literature (σΔlog(O/H) = 0.07
dex). Indeed, this dispersion is only slightly higher than the typical
error derived for our oxygen abundances. However, we found no secondary
relation with the star-formation rate other than the one induced by the
primary relation of this quantity with the stellar mass. The analysis
for our sample of ~3000 individual HII regions confirms (i) a local
mass-metallicity relation and (ii) the lack of a secondary relation with
the star-formation rate. The same analysis was performed with similar
results for the specific star-formation rate.
Our results agree with the scenario in which gas recycling in galaxies,
both locally and globally, is much faster than other typical timescales,
such like that of gas accretion by inflow and/or metal loss due to
outflows. In essence, late-type/disk-dominated galaxies seem to be in a
quasi-steady situation, with a behavior similar to the one expected from
an instantaneous recycling/closed-box model.
Table 1 and Appendix A are available in electronic form at www.aanda.org.
- Organisation(s)
- Department of Astrophysics
- External organisation(s)
- Instituto de Astrofísica de Andalucía (CSIC), Universidad Autónoma de Madrid, Czech Academy of Sciences, Leibniz-Institut für Astrophysik Potsdam, Universidad Complutense de Madrid, Centro Astronómico Hispano Alemán (CAHA), Universidade Federal de Santa Catarina, Instituto Superior Técnico, Max-Planck-Institut für Astronomie, The University of Sydney, Australian Astronomical Observatory, Centro de Investigaciones Energeticas Medioambientales y Tecnológica, University of Copenhagen, Universidade do Porto, University of Sheffield, Universidad de Granada, University of La Laguna, Institute of Astrophysics of the Canary Islands, Landessternwarte Königstuhl (LSW), Ruhr-Universität Bochum (RUB), National Institute of Astrophysics, Optics and Electronics (INAOE), Université de recherche Paris Sciences et Lettres
- Journal
- Astronomy & Astrophysics
- Volume
- 554
- No. of pages
- 8
- ISSN
- 0004-6361
- DOI
- https://doi.org/10.1051/0004-6361/201220669
- Publication date
- 06-2013
- Peer reviewed
- Yes
- Austrian Fields of Science 2012
- 103004 Astrophysics, 103003 Astronomy
- Keywords
- Portal url
- https://ucrisportal.univie.ac.at/en/publications/1f3eb916-13aa-48b8-b194-a93aebea5773