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The Evolution of the Mass–Metallicity Relation in Seyferts

Published online by Cambridge University Press:  03 June 2010

N. Vale Asari ,
G. Stasińska ,
R. Cid Fernandes ,
J. M. Gomes ,
M. Schlickmann ,
A. Mateus  and
W. Schoenell
N. Vale Asari
Affiliation:
Dpto. de Física - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; Place Jules Janssen 92190 Meudon, France
G. Stasińska
Affiliation:
LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; Place Jules Janssen 92190 Meudon, France
R. Cid Fernandes
Affiliation:
Dpto. de Física - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil
J. M. Gomes
Affiliation:
Dpto. de Física - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil GEPI, Observatoire de Paris, CNRS, Université Paris Diderot; Place Jules Janssen 92190 Meudon, France
M. Schlickmann
Affiliation:
Dpto. de Física - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil
A. Mateus
Affiliation:
IAG, Universidade de São Paulo, São Paulo, SP, Brazil
W. Schoenell
Affiliation:
Dpto. de Física - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil
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Various studies have shown that there is an empirical relation between the nebular metallicity of a galaxy and its stellar mass. Until now, most studies of the mass-metallicity relation (M–Z) have focused on the abundances of the interstellar medium as measured by emission-line features. This technique thus excludes galaxies with AGN from the working samples, due to the difficulty to measure the nebular abundances when emission-lines are powered both by stars and AGN. With our synthesis code starlight, we are able to recover the stellar metallicities of galaxies from the Sloan Digital Sky Survey (SDSS). Therefore, although we still cannot measure the nebular metallicity in AGN hosts, we know their present-day stellar metallicities. Moreover, because we measure the metallicity of stellar populations of different ages in a galaxy, we are also able also recover the history of its chemical enrichment.

Keywords

galaxies: evolutiongalaxies: statisticsgalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 144
Copyright
Copyright © International Astronomical Union 2010

References

Vale Asari, N., Stasińska, G., Cid Fernandes, R., Gomes, J. M., Schlickmann, M., Mateus, A., & Schoenell, W. 2009, MNRAS, 396, L71CrossRefGoogle Scholar