具有$0<z<5$的类星体中\civ Baldwin效应的潜在驱动因素
The underlying driver for the \civ Baldwin effect in QSOs with $0<z<5$
摘要：
宽发射谱线是第一类类星体的一个显著特征。\civ $\lambda1549~$的Baldwin效应起源于宽发射线，即，\civ等效宽度（EW）的亮度依赖性没有被清楚地建立。利用87个低$z$ Palomar-Green（PG）类星体和126个高$z$类星体的样本，在最宽的可能红移范围（$0<z<5$）内，我们一致地计算了基于\hb的单历元超大质量黑洞（SMBH）质量和爱丁顿比，以研究\civ Baldwin效应的潜在驱动因素。本文提出了一个估算5100 nm连续光度中主体部分的经验公式，并用于基于\hb的低$z$ PG类星体的\mbh计算.通过主成分分析发现，对于低$z$ PG类星体，爱丁顿比与PC 1和PC 2有很强的相关性，而\civ EW与光学\feii强度或PC 1有很强的相关性。将高$z$类星体的光度范围扩大，发现在我们的类星体样本中存在\civ Baldwin效应.用基于\hb的单历元SMBH质量对我们的类星体样本进行分析，发现\civ EW与爱丁顿比的相关性比SMBH质量的相关性强。这意味着，爱丁顿比似乎是一个更好的基本参数比SMBH质量驱动的\civ鲍德温效应。
英文摘要：
Broad emission lines is a prominent property of type I quasi-stellar objects (QSOs). The origin of the Baldwin effect for \civ $\lambda1549~$Å broad emission lines, i.e., the luminosity dependence of the \civ equivalent width (EW), is not clearly established. Using a sample of 87 low-$z$ Palomar-Green (PG) QSOs and 126 high-$z$ QSOs across the widest possible ranges of redshift ($0<z<5$), we consistently calculate \hb-based single-epoch supermassive black hole (SMBH) mass and the Eddington ratio to investigate the underlying driver of the \civ Baldwin effect. An empirical formula to estimate the host fraction in the continuum luminosity at 5100 Å is presented and used in \hb-based \mbh calculation for low-$z$ PG QSOs. It is found that, for low-$z$ PG QSOs, the Eddington ratio has strong correlations with PC1 and PC2 from the principal component analysis, and \civ EW has a strong correlation with the optical \feii strength or PC1. Expanding the luminosity range with high-$z$ QSOs, it is found that \civ Baldwin effect exists in our QSOs sample. Using \hb-based single-epoch SMBH mass for our QSOs sample, it is found that \civ EW has a strong correlation with the Eddington ratio, which is stronger than that with the SMBH mass. It implies that the Eddington ratio seems to be a better underlying parameter than the SMBH mass to drive the \civ Baldwin effect.
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