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Metallicity of the high-redshift Universe traced by radio galaxies

Published online by Cambridge University Press:  09 March 2010

K. Matsuoka ,
T. Nagao ,
R. Maiolino ,
A. Marconi  and
Y. Taniguchi
K. Matsuoka
Affiliation:
Graduate School of Science and Engineering, Ehime University, 2-5 Bunkyo-cho, Matsuyama 790-8577, Japan email: [email protected]
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Abstract

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We investigate the metallicity of the narrow line regions (NLRs) of high-z radio galaxies (HzRGs), using new deep optical spectra of 9 HzRGs obtained with FORS2 on VLT and data from the literature. To estimate the metallicity of NLRs we focus on the Civ/Heii and Ciii]/Civ flux ratios. Based on comparison between the observed emission-line flux ratios and the prediction of our photoionization model calculations, we find no significant metallicity evolution in NLRs of HzRGs, up to z ~ 4. We discuss the possibility that massive galaxies had almost completed the major epoch of the star formation in the very high-z universe (z > 5).

Keywords

galaxies: activegalaxies: evolutionquasars: emission linesquasars: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 179 - 180
Copyright
Copyright © International Astronomical Union 2010

References

Ferland, G. J., Korista, K. T., Verner, D. A., et al. 1998, PASP, 110, 761CrossRefGoogle Scholar
Maiolino, R., Nagao, T., Grazian, A., et al. 2008, A&A, 488, 463Google Scholar
Matsuoka, K., Nagao, T., Maiolino, R., et al. 2009, A&A, 503, 721Google Scholar
Nagao, T., Maiolino, R., & Marconi, A. 2006, A&A, 447, 863Google Scholar