Journal Article

The black hole mass–stellar velocity dispersion correlation: bulges versus pseudo-bulges

Jian Hu

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 386, issue 4, pages 2242-2252
Published in print June 2008 | ISSN: 0035-8711
Published online April 2008 | e-ISSN: 1365-2966 | DOI:
The black hole mass–stellar velocity dispersion correlation: bulges versus pseudo-bulges

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We investigate the correlation between the supermassive black holes (SMBHs) mass (Mbh) and the stellar velocity dispersion (σ*) in two types of host galaxies: the early-type bulges (disc galaxies with classical bulges or elliptical galaxies) and pseudo-bulges. In the form log (Mbh/M) =α+β log (σ*/200 km s−1), the best-fitting results for the 39 early-type bulges are the slope β= 4.06 ± 0.28 and the normalization α= 8.28 ± 0.05; the best-fitting results for the nine pseudo-bulges are β= 4.5 ± 1.3 and α= 7.50 ± 0.18. Both relations have intrinsic scatter in log Mbh of ≲0.27 dex. The Mbh–σ* relation for pseudo-bulges is different from the relation in the early-type bulges over the 3σ significance level. The contrasting relations indicate the formation and growth histories of SMBHs depend on their host type. The discrepancy between the slope of the Mbh–σ* relations using different definition of velocity dispersion vanishes in our sample, a uniform slope will constrain the coevolution theories of the SMBHs and their host galaxies more effectively. We also find the slope for the ‘core’ elliptical galaxies at the high-mass range of the relation appears steeper (β≃ 5–6), which may be the imprint of their origin of dissipationless mergers.

Keywords: black hole physics; galaxies: bulges; galaxies: formation; galaxies: fundamental parameters; galaxies: nuclei

Journal Article.  8139 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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