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Black hole growth and the MBH–bulge relations

Published online by Cambridge University Press:  01 December 2004

Smita Mathur  and
Dirk Grupe
Smita Mathur
Affiliation:
Astronomy Department, The Ohio State University, 140 West 18th Ave., Columbus, OH 43210, USA email: smita@astronomy.ohio-state.edu
Dirk Grupe
Affiliation:
Astronomy Department, The Ohio State University, 140 West 18th Ave., Columbus, OH 43210, USA email: smita@astronomy.ohio-state.edu
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Abstract

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We present the black hole mass–bulge velocity dispersion relation for a complete sample of 75 soft X-ray selected AGNs. We find that the AGNs with highest accretion rates relative to Eddington lie below the MBH–σ relation of broad line Seyfert 1s, confirming the Mathur et al. (2001) result. The statistical result is robust and not due to any systematic measurement error. This has important consequences towards our understanding of black hole formation and growth: black holes grow by accretion in well formed bulges. As they grow, they get closer to the MBH–σ relation for normal galaxies. The accretion is highest in the beginning and dwindles as time goes by. Our result does not support theories of the MBH–σ relation in which the black hole mass is a constant fraction of the bulge mass/velocity dispersion at all times or those in which bulge growth is controlled by AGN feedback.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 501 - 504
Copyright
© 2004 International Astronomical Union