The distribution of supermassive black holes in the nuclei of nearby galaxies

被引：89
|
作者：
Cattaneo, A
Haehnelt, MG
Rees, MJ
机构：
[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[2] Max Planck Inst Astrophys, D-85740 Garching, Germany
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 1999年 / 308卷 / 01期
关键词：
black hole physics; galaxies : formation; galaxies : nuclei; quasars : general;
D O I：
10.1046/j.1365-8711.1999.02693.x
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The growth of supermassive black holes by merging and accretion in hierarchical models of galaxy formation is studied by means of Monte Carlo simulations. A tight linear relation between masses of black holes and masses of bulges arises if the mass accreted by supermassive black holes scales linearly with the mass-forming stars and if the redshift evolution of mass accretion tracks closely that of star formation. Differences in redshift evolution between black hole accretion and star formation introduce a considerable scatter in this relation. A non-linear relation between black hole accretion and star formation results in a non-linear relation between masses of remnant black holes and masses of bulges. The relation of black hole mass to bulge luminosity observed in nearby galaxies and its scatter are reproduced reasonably well by models in which black hole accretion and star formation are linearly related but do not track each other in redshift. This suggests that a common mechanism determines the efficiency for black hole accretion and the efficiency for star formation, especially for bright bulges.
引用
收藏
页码：77 / 81
页数：5
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