The Lick AGN Monitoring Project 2011: Dynamical Modeling of the Broad-line Region
The Lick AGN Monitoring Project 2011: Dynamical Modeling of the Broad-line Region
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DOI：
10.3847/1538-4357/aae086
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发表时间：
2018-09
期刊：
影响因子：
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通讯作者：
P. Williams;A. Pancoast;T. Treu;B. Brewer;A. Barth;V. Bennert;Tabitha Buehler;G. Canalizo
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文献类型：
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作者：
P. Williams;A. Pancoast;T. Treu;B. Brewer;A. Barth;V. Bennert;Tabitha Buehler;G. Canalizo
我们提出了来自Lick AGN监测项目2011样本的7个Seyfert 1星系的Hβ发射宽线区（BLR）模型，对BLR结构和动力学以及中心超大质量黑洞的质量进行了推断。我们发现，BLR一般是一个厚盘，靠近正面，优先发射回电离源。我们样本中的动态范围从近圆形椭圆轨道到流入或流出轨道。我们测量了PG 1310−108、Mrk 50、Mrk 141、Mrk 279、Mrk 1511、NGC 4593和Zw 229−015的黑洞质量。我们使用这些黑洞质量测量沿着与互相关时间滞后和线宽恢复的比例因子f在传统的混响映射测量。将我们的结果与使用这种建模技术的其他研究相结合，使我们的样本量达到16，我们计算出一个比例因子，可用于在其他混响映射活动中测量黑洞质量。当使用均方根（rms）谱和使用线色散来测量线宽时，我们发现pred = 0.57 ± 0.19。最后，我们寻找f和其他活动星系核和BLR参数之间的相关性，并找到边缘的证据表明，f与MBH和BLR倾角，但没有显着的证据与活动星系核的光度或爱丁顿比的相关性。
We present models of the Hβ-emitting broad-line region (BLR) in seven Seyfert 1 galaxies from the Lick AGN Monitoring Project 2011 sample, drawing inferences on the BLR structure and dynamics as well as the mass of the central supermassive black hole. We find that the BLR is generally a thick disk, viewed close to face-on, with preferential emission back toward the ionizing source. The dynamics in our sample range from near-circular elliptical orbits to inflowing or outflowing trajectories. We measure black hole masses of for PG 1310−108, for Mrk 50, for Mrk 141, for Mrk 279, for Mrk 1511, for NGC 4593, and for Zw 229−015. We use these black hole mass measurements along with cross-correlation time lags and line widths to recover the scale factor f used in traditional reverberation mapping measurements. Combining our results with other studies that use this modeling technique, which brings our sample size to 16, we calculate a scale factor that can be used for measuring black hole masses in other reverberation mapping campaigns. When using the root-mean-square (rms) spectrum and using the line dispersion to measure the line width, we find pred = 0.57 ± 0.19. Finally, we search for correlations between f and other AGN and BLR parameters and find marginal evidence that f is correlated with MBH and the BLR inclination angle, but no significant evidence of a correlation with the AGN luminosity or Eddington ratio.