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The stellar populations in low excitation and high excitation radio galaxies

Published online by Cambridge University Press:  17 July 2013

Michael B. Pracy ,
John Ching ,
Scott Croom  and
Elaine M. Sadler
Michael B. Pracy
Affiliation:
Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW, 2006, Australia email: mpracy@physics.usyd.edu.au
John Ching
Affiliation:
Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW, 2006, Australia email: mpracy@physics.usyd.edu.au
Scott Croom
Affiliation:
Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW, 2006, Australia email: mpracy@physics.usyd.edu.au
Elaine M. Sadler
Affiliation:
Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW, 2006, Australia email: mpracy@physics.usyd.edu.au
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Abstract

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We have conducted deep optical spectroscopic follow up of a sample of radio galaxies with redshifts z < 0.7. The spectra were used to construct robust sub-samples of low excitation and high excitation AGN and perform stellar population analysis via line indices and spectral fitting. While the high excitation objects have lower luminosity-weighted ages and lower metallicities than the low excitation galaxies, this can be explained by the different stellar mass distributions of the samples. When stellar mass is taken into account the age and metallicity distribution of both populations are consistent with the galaxy population as a whole.

Keywords

galaxies: activegalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S295: The intriguing life of massive galaxies , August 2012 , pp. 117 - 120
Copyright
Copyright © International Astronomical Union 2013 

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