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Co-Evolution of Supermassive Black Holes and Their Host Galaxies

Published online by Cambridge University Press:  03 June 2010

J. K. Kotilainen ,
R. Decarli ,
R. Falomo ,
A. Treves ,
M. Labita  and
R. Scarpa
J. K. Kotilainen
Affiliation:
Finnish Centre for Astronomy with ESO (FINCA) and Tuorla Observatory, University of Turku, FI-21500 Piikkiö, Finland Email: jarkot@utu.fi
R. Decarli
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
R. Falomo
Affiliation:
INAF – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
A. Treves
Affiliation:
Università dell'Insubria, via Valleggio 11, I-22100 Como, Italy
M. Labita
Affiliation:
Università dell'Insubria, via Valleggio 11, I-22100 Como, Italy
R. Scarpa
Affiliation:
Instituto de Astrofisica de Canarias, C/ Via Lactea, s/n E38205 – La Laguna, Tenerife, Spain
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Abstract

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We study the evolution of the MBH/Mhost relation up to z = 3 for a sample of 96 quasars with known host galaxy luminosities. Black hole masses are estimated assuming virial equilibrium in the broad-line regions, while the host galaxy masses are inferred from their luminosities. With this data, we are able to pin down the evolution of the MBH/Mhost relation over 85% of the age of the universe. While the MBH/Lhost relation remains nearly unchanged, taking into account the aging of the stellar population, we find that the MBH/Mhost ratio (Γ) increases by a factor ~ 7 from z = 0 to z = 3. We show that the evolution of Γ is independent of radio loudness and quasar luminosity. We propose that the most massive black holes, in their quasar phase at high-redshift, become extremely rare objects in host galaxies of similar mass in the local universe.

Keywords

galaxies: activegalaxies: evolutiongalaxies: high-redshiftgalaxies: nuclei (galaxies:) quasars: general
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. 34 - 39
Copyright
Copyright © International Astronomical Union 2010

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