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Chemical evolution of Seyfert galaxies

Published online by Cambridge University Press:  01 July 2007

Silvia K. Ballero ,
Francesca Matteucci  and
Luca Ciotti
Silvia K. Ballero
Affiliation:
Dipartimento di Astronomia, Università di Trieste, via G.B. Tiepolo 11, 34124 Trieste, Italy INAF, Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34124 Trieste, Italy
Francesca Matteucci
Affiliation:
Dipartimento di Astronomia, Università di Trieste, via G.B. Tiepolo 11, 34124 Trieste, Italy INAF, Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34124 Trieste, Italy
Luca Ciotti
Affiliation:
Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127, Bologna, Italy
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Abstract

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We computed the chemical evolution of Seyfert galaxies, residing in spiral bulges, based on an updated model for the Milky Way bulge with updated calculations of the Galactic potential and of the feedback from the central supermassive black hole (BH) in a spherical approximation. We followed the evolution of bulges of masses 2 × 109 − 1011M⊙ by scaling the star-formation efficiency and the bulge scalelenght as in the inverse-wind scenario for ellipticals. We successfully reproduced the observed relation between the BH mass and that of the host bulge, and the observed peak nuclear bolometric luminosity. The observed metal overabundances are easily achieved, as well as the constancy of chemical abundances with the redshift.

Keywords

Galaxy: bulgegalaxies: abundancesgalaxies: evolutiongalaxies: Seyfert
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 231 - 232
Copyright
Copyright © International Astronomical Union 2008

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