A Comparison of Stellar and Gaseous Kinematics in the Nuclei of Active Galaxies
A Comparison of Stellar and Gaseous Kinematics in the Nuclei of Active Galaxies
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DOI：
10.1086/430590
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发表时间：
2005-03
期刊：
影响因子：
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通讯作者：
Jenny E. Greene;L. C. Ho
中科院分区：
文献类型：
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作者：
Jenny E. Greene;L. C. Ho
为了研究黑洞与其宿主星系之间的关系，许多研究小组使用[O III] λ5007线的宽度作为星系凸起的恒星速度色散（σ*）的替代。我们直接测试这一假设与一个大的和均匀的样本窄线活动星系核从斯隆数字巡天。我们考虑多个跃迁（[O II] λ3727，[O III] λ5007和[S II] λλ6716，6731）和各种技术来量化线宽，以获得气体速度色散σg和σ* 之间的校准。我们发现低电离线的σg追踪σ*，在适当去除不对称蓝翼后，[O III]核心的σg也追踪σ *，尽管在所有情况下，σg和σ* 之间的相关性都有相当大的分散。虽然气体运动的窄线区域的活动星系主要是由恒星的引力势，吸积率，跟踪爱丁顿光度比，似乎发挥了重要的次要作用。维里运动的结果与吸积速率有系统的相关性。我们讨论了这些结果的影响，以前的研究，使用[O III]线宽度来推断恒星的速度色散类星体和窄线塞弗特1星系。
To investigate the relationship between black holes and their host galaxies, many groups have used the width of the [O III] λ5007 line as a substitute for the stellar velocity dispersion (σ*) of galaxy bulges. We directly test this assumption with a large and homogeneous sample of narrow-line active galactic nuclei from the Sloan Digital Sky Survey. We consider multiple transitions ([O II] λ3727, [O III] λ5007, and [S II] λλ6716, 6731) and various techniques for quantifying the line width in order to obtain a calibration between the gas velocity dispersion, σg, and σ*. We find that σg of the low-ionization lines traces σ*, as does σg for the core of [O III] after its asymmetric blue wing is properly removed, although in all cases the correlation between σg and σ* has considerable scatter. While the gas kinematics of the narrow-line region of active galaxies are primarily governed by the gravitational potential of the stars, the accretion rate, as traced by the Eddington luminosity ratio, seems to play an important secondary role. Departures from virial motions correlate systematically with accretion rate. We discuss the implications of these results for previous studies that use [O III] line widths to infer stellar velocity dispersions in quasars and narrow-line Seyfert 1 galaxies.