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The correlation between black hole mass and bulge velocity dispersion in hierarchical galaxy formation models
Astrophysics · Submitted 25 Jul 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We conclude that the small scatter in the observed M_bh - sigma relation is consistent with a picture in which bulges and black holes form over a wide range in redshift.
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The abstract, sentence by sentence
Recent work has demonstrated that there is a tight correlation between the mass of a black hole and the velocity dispersion of the bulge of its host galaxy. We show that the model of Kauffmann & Haehnelt, in which bulges and supermassive black holes both form during major mergers, produces a correlation between M_bh and sigma with slope and scatter comparable to the observed relation. In the model, the M_bh - sigma relation is significantly tighter than the correlation between black hole mass and bulge luminosity or the correlation between bulge luminosity and velocity dispersion. There are two reasons for this: i) the gas masses of bulge progenitors depend on the velocity dispersion but not on the formation epoch of the bulge, whereas the stellar masses of the progenitors depend on both; ii) mergers between galaxies move black holes along the observed M_bh - sigma relation, even at late times when the galaxies are gas-poor and black holes grow mainly by merging of pre-existing black holes. We conclude that the small scatter in the observed M_bh - sigma relation is consistent with a picture in which bulges and black holes form over a wide range in redshift.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Recent work has demonstrated that there is a tight correlation between the mass of a black hole and the velocity dispersion of the bulge of its host galaxy. | background 1.00 | 0.03 | 0.04 | asserted 1.00 |
| s1 | We show that the model of Kauffmann & Haehnelt, in which bulges and supermassive black holes both form during major mergers, produces a correlation between M_bh and sigma with slope and scatter comparable to the observed relation. | result 0.75 | 0.94 | 0.29 | asserted 1.00 |
| s2 | In the model, the M_bh - sigma relation is significantly tighter than the correlation between black hole mass and bulge luminosity or the correlation between bulge luminosity and velocity dispersion. | result 1.00 | 0.87 | 0.13 | asserted 1.00 |
| s3 | There are two reasons for this: i) the gas masses of bulge progenitors depend on the velocity dispersion but not on the formation epoch of the bulge, whereas the stellar masses of the progenitors depend on both; ii) mergers between galaxies move black holes along the observed M_bh - sigma relation, even at late times when the galaxies are gas-poor and black holes grow mainly by merging of pre-existing black holes. | interpretation 0.93 | 0.73 | 0.08 | asserted 1.00 |
| s4 | We conclude that the small scatter in the observed M_bh - sigma relation is consistent with a picture in which bulges and black holes form over a wide range in redshift. | interpretation 0.99 | 0.65 | 0.92 | hedged possibility 1.00 |
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Original abstract
Recent work has demonstrated that there is a tight correlation between the mass of a black hole and the velocity dispersion of the bulge of its host galaxy. We show that the model of Kauffmann & Haehnelt, in which bulges and supermassive black holes both form during major mergers, produces a correlation between M_bh and sigma with slope and scatter comparable to the observed relation. In the model, the M_bh - sigma relation is significantly tighter than the correlation between black hole mass and bulge luminosity or the correlation between bulge luminosity and velocity dispersion. There are two reasons for this: i) the gas masses of bulge progenitors depend on the velocity dispersion but not on the formation epoch of the bulge, whereas the stellar masses of the progenitors depend on both; ii) mergers between galaxies move black holes along the observed M_bh - sigma relation, even at late times when the galaxies are gas-poor and black holes grow mainly by merging of pre-existing black holes. We conclude that the small scatter in the observed M_bh - sigma relation is consistent with a picture in which bulges and black holes form over a wide range in redshift.
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