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Black Holes, Galaxy Formation, and the M BH - Relation

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King, Andrew·2003·The Astrophysical Journal

Abstract

Recent X-ray observations of intense high-speed outflows in quasars suggest that supercritical accretion on to the central black hole may have an important effect on a host galaxy. I revisit some ideas of Silk & Rees and assume that such flows occur in the final stages of building up the black hole mass. It is now possible to model explicitly the interaction between the outflow and the host galaxy. This is found to resemble a momentum-driven stellar wind bubble, implying a relation M BH = ( f g κ/2π G 2 )σ 4 ≃ 1.5 × 10 8 σ M ☉ between black hole mass and bulge velocity dispersion ( f g = gas fraction of total matter density, κ = electron scattering opacity), without free parameters. This is remarkably close to the observed relation in both slope and normalization. This result suggests that the central black holes in galaxies gain most of their mass in phases of super-Eddington accretion, which are presumably obscured or at high redshift. Observed super-Eddington quasars are apparently late in growing their black hole masses.

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Metadata

Authors
King, A.
Venue
The Astrophysical Journal
Published
2003-09-15
Volume
596
Issue
1
Pages
L27-L29
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2034343521
Cited by
805
References
2
FWCI
12.56
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: Black Holes, Galaxy Formation, and the M BH - Relation. https://app.cochat.ai/papers/10.1086/379143
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King, A. (2003). Black Holes, Galaxy Formation, and the M BH - Relation. The Astrophysical Journal. https://doi.org/10.1086/379143

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

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