Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. VIII. Structure of the Broad-line Region and Mass of the Central Black Hole in Mrk 142
Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. VIII. Structure of the Broad-line Region and Mass of the Central Black Hole in Mrk 142
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DOI：
10.3847/1538-4357/aaee6b
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发表时间：
2018-11
期刊：
影响因子：
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通讯作者：
Yan-Rong Li;Yu-Yang Songsheng;Jie Qiu;Chen Hu;P. Du;K. Lu;Ying-Ke Huang;J. Bai;W. Bian
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文献类型：
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作者：
Yan-Rong Li;Yu-Yang Songsheng;Jie Qiu;Chen Hu;P. Du;K. Lu;Ying-Ke Huang;J. Bai;W. Bian
这是一系列报道大型混响映射（RM）活动的论文中的第八篇，该活动旨在测量具有高吸积率的活动星系核中的黑洞（BH）质量。我们采用最近开发的基于Pancoast等人方法的宽线区域（blr）动态建模方法来分析Mrk 142在第一个监测季节观测到的RM数据集。在这种方法中，使用阻尼随机游走过程重建连续体变化，并使用灵活的盘状几何形状描绘BLR结构，其中BLR云以开普勒轨道或流入/流出运动围绕BH中心移动。该方法还包括BLR云各向异性发射的可能性、线发射对连续体的非线性响应、连续体的不同长期趋势和发射在线变化。我们在适合并行计算的贝叶斯框架中实现该方法，并使用马尔可夫链蒙特卡罗技术来恢复建模的参数和不确定性，包括中心黑洞的质量。我们应用了三种不同BLR云分布处方的BLR模型，发现适合Mrk 142数据的最佳模型是两区BLR模型，与围绕薄吸积盘的理论BLR模型一致。最好的模型产生的黑洞质量为，导致从平均光谱测量到的Hβ线的全宽度最大一半处的维里因子为。本文还介绍了其他测量Hβ线宽的维里因子。
This is the eighth in a series of papers reporting on a large reverberation mapping (RM) campaign to measure black hole (BH) mass in active galactic nuclei with high accretion rates. We employ the recently developed dynamical modeling approach for broad-line regions (BLRs) based on the method of Pancoast et al. to analyze the RM data set of Mrk 142 observed in the first monitoring season. In this approach, continuum variations are reconstructed using a damped random walk process, and BLR structure is delineated using a flexible disk-like geometry, in which BLR clouds move around the central BH with Keplerian orbits or inflow/outflow motion. The approach also includes the possibilities of anisotropic emission from BLR clouds, nonlinear response of the line emission to the continuum, and different long-term trends in the continuum and emission-line variations. We implement the approach in a Bayesian framework that is apt for parallel computation and use a Markov chain Monte Carlo technique to recover the parameters and uncertainties for the modeling, including the mass of the central BH. We apply three BLR models with different prescriptions of BLR cloud distributions and find that the best model for fitting the data of Mrk 142 is a two-zone BLR model, consistent with the theoretical BLR model surrounding slim accretion disks. The best model yields a BH mass of , resulting in a virial factor of for the full width at half maximum of the Hβ line measured from the mean spectrum. The virial factors for the other measures of the Hβ line width are also presented.