The black hole–bulge relation in active galactic nuclei
The black hole–bulge relation in active galactic nuclei
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DOI：
10.1111/j.1365-2966.2004.07233.x
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发表时间：
2003-09
影响因子：
4.8
通讯作者：
W. Bian;Yinghe Zhao
中科院分区：
文献类型：
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作者：
W. Bian;Yinghe Zhao
利用Hβ和[O III]发射线的宽度研究了射电强活动星系核（AGN）、射电静活动星系核（AGN）和窄线Seyfert I星系（NLS 1 s）中黑洞-球核的关系。中心黑洞质量M bh由Hβ谱线宽度和光学光度估算，而核球速度色散a则由[O III]谱线宽度直接估算。我们发现，射电宁静活动星系核遵循邻近不活跃星系的M bh -σ关系，而射电强活动星系核和NLS 1则偏离了这一关系。对于射电活动星系核的偏离有两种可能的解释。一种是由于高估了光学亮度，因此高估了发射HAS线的宽线区域（BLR）的大小。二是射电强活动星系核中BLR和/或窄线区的动力学特征与射电静活动星系核中的不同。NLS 1 s的偏差可能是由于BLR对视线的小倾斜或[O III]线宽作为恒星速度色散指标的可靠性，因为它的复杂的多个组件。
We have used the widths of Hβ and [O III] emission lines to investigate the black hole-bulge relation in radio-loud active galactic nuclei (AGNs), radio-quiet AGNs and narrow-line Seyfert I galaxies (NLS1s). The central black hole mass, M bh , is estimated from the Hβ linewidth and the optical luminosity, and the bulge velocity dispersion, a, is directly estimated from the width of the [O III] line. We have found that radio-quiet AGNs follow the established M bh -σ relationship in nearby inactive galaxies, while radio-loud AGNs and NLS1s deviate from this relationship. There are two plausible interpretations for the deviation of radio-loud AGNs. One is that the size of broad-line regions (BLRs) emitting the HAS line is overestimated because of the overestimation of optical luminosity. The other is that the dynamics of BLRs and/or narrow-line regions in radio-loud AGNs is different from that in radio-quiet AGNs. The deviation of NLS1s may be due to the small inclination of BLRs to the line of sight or the reliability of the [O III] linewidth as the indicator of stellar velocity dispersion because of its complex multiple components.