A CORRELATION BETWEEN CENTRAL SUPERMASSIVE BLACK HOLES AND THE GLOBULAR CLUSTER SYSTEMS OF EARLY-TYPE GALAXIES
A CORRELATION BETWEEN CENTRAL SUPERMASSIVE BLACK HOLES AND THE GLOBULAR CLUSTER SYSTEMS OF EARLY-TYPE GALAXIES
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DOI：
10.1088/0004-637x/720/1/516
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发表时间：
2010-04
期刊：
影响因子：
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通讯作者：
A. Burkert;S. Tremaine
中科院分区：
文献类型：
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作者：
A. Burkert;S. Tremaine
椭圆星系、透镜星系和早型旋涡星系的中心超大质量黑洞（SMBH）的质量M·与球状星团（GC）的数目NGC之间存在着非常紧密的幂律关系：M· = m·/N × N1.08±0.04GC，其中m·/N = 1.7 × 105 M·t。因此，为了良好的近似，SMBH质量与GC的总质量相同。基于有限的13个星系的样本，这个关系似乎是一个更好的预测SMBH质量（均方根散射0.2 dex）比SMBH质量和速度色散σ之间的M·-σ关系。小的散射反映了这样一个事实，即具有高GC比频率SN的星系倾向于拥有比M·-σ关系所预期的更大质量的SMBH。
Elliptical, lenticular, and early-type spiral galaxies show a remarkably tight power-law correlation between the mass M• of their central supermassive black hole (SMBH) and the number NGC of globular clusters (GCs): M• = m•/⋆ × N1.08±0.04GC with m•/⋆ = 1.7 × 105 M☉. Thus, to a good approximation the SMBH mass is the same as the total mass of the GCs. Based on a limited sample of 13 galaxies, this relation appears to be a better predictor of SMBH mass (rms scatter 0.2 dex) than the M•–σ relation between SMBH mass and velocity dispersion σ. The small scatter reflects the fact that galaxies with high GC specific frequency SN tend to harbor SMBHs that are more massive than expected from the M•–σ relation.