论文标题
活性银河核的光学\ FEII发射与无量纲增生率之间的关系
The Relation between the Optical \feii Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
论文作者
论文摘要
有人提出，光学Fe II发射的显着特征与活性银河核（AGN）中的积聚过程有联系。对于大量的4037类品类（$ z <0.8 $），并测量了$ \ rmhβ$线的分散（$σ_{\ rmhβ} $），从斯隆数字天空调查（SDSS）和120个收集的Reverberation Reverberation-Mappation（RM）Agn中，我们使用$ = _ _ \ rmhβ} Blr} -l _ {\ rm 5100} $从SDSS subsampe的单上观测光谱和$σ_ {\ rmHβ} $中的单点光谱中计算出超大型黑洞质量（$ m _ {\ rm bh} $）。我们发现相对光学Fe II强度$ r _ {\ rm fe} $与$ \ dot {\ nathscr {m}} $的$ \ dot {\ mathscr {m}} $，用于SDSS子样本，带有Spearman相关系数$ r_s $ $ r_s $ $ 0.727 $，这与从平均subsplem subsmple中获得的相一致。每当有流入或流出时，光学Fe II发射的速度偏移的幅度就具有强大的反相关性。这些强相关性表明，光学Fe II发射与积聚过程有着密切的联系。假设$ m _ {\ rm bh} $的差异是由于采用$ \ rm fwhm_ {hβ} $作为速度示踪剂的可变病毒因子$ f $引起fwhm _ {\ rmHβ}+（1.719 \ pm 0.009）$用于单两个光谱。 $ \ log f $和$σ_{\ rmhβ} $之间的关系并不太强，这表明$σ_{\ rmhβ} $似乎不大取决于宽线区域的倾斜度，并且基于$σ$ f $的常数$σ$ f $适合$ f $，适合$σ__ {\ rmHβ} $ as velacity。
It was suggested that the prominent feature of the optical Fe II emission has a connection with the accretion process in active galactic nuclei (AGN). For a large sample of 4037 quasars ($z < 0.8$) with measured $\rm Hβ$ line dispersion ($σ_{\rm Hβ}$) selected from the Sloan Digital Sky Survey (SDSS) and 120 compiled reverberation-mapped (RM) AGN, we use $σ_{\rm Hβ}$ and the extended $R_{\rm BLR}-L_{\rm 5100}$ relation to calculate supermassive black holes masses ($M_{\rm BH}$) from the single-epoch spectra for the SDSS subsample, and $σ_{\rm Hβ}$ from the mean spectra for the RM subsample. We find a strong correlation between the relative optical Fe II strength $R_{\rm Fe}$ and $\dot{\mathscr{M}}$ for the SDSS subsample with the Spearman correlation coefficient $r_s$ of $0.727$, which is consistent with that derived from the mean spectra for the RM subsample. The magnitude of velocity shift of the optical Fe II emission has a strong anticorrelation with $\dot{\mathscr{M}}$, whenever there is inflow or outflow. These strong correlations show that the optical Fe II emission has an intimate connection with the accretion process. Assuming that the difference of $M_{\rm BH}$ is due to the variable virial factor $f$ for adopting $ \rm FWHM_{Hβ}$ as the velocity tracer, we find that there is a relation between $f$ and $\rm FWHM_{Hβ}$, $\log f=-(0.41\pm 0.002) \rm \log FWHM_{\rm Hβ}+(1.719\pm 0.009)$ for the single-epoch spectrum. The relation between $\log f$ and $σ_{\rm Hβ}$ is not too strong, suggesting that $σ_{\rm Hβ}$ does not seem to depend much on the broad-line region inclination and a constant $σ$-based $f$ is suitable for $σ_{\rm Hβ}$ as the velocity tracer.
