In this paper we study the properties of the optical spectra of Type 1 active galactic nuclei (AGNs) by using the unobscured hard X-ray emission as a diagnostic. We develop the `Correlation Spectrum Technique' (CST) and use this to show the strength of correlation between the hard X-ray luminosity and each wavelength of the optical spectrum. This shows that for Broad Line Seyfert 1s all the strong emission lines (broad component of Hαand Hβ, [NeIII] λλ3869/3967, [OI] λλ6300/6364, [OII] λλ3726/3729, [OIII] λλ4959/5007) and the optical underlying continuum all strongly correlate with the hard X-ray emission. But the NLS1s appear to be somewhat different. Among the various Balmer line components and the broadband SED components, the best correlation exists between the hard X-ray component and broad component (BC) of the Balmer lines, which supports the view that broad line region (BLR) has the closest link with the AGN's compact X-ray emission. The equivalent widths of Balmer line IC and BC are found to correlate with L$_{2-10keV}$, $κ_{2-10keV}^{-1} = L_{bol}/L_{2-10keV}$, Balmer line FWHM and black hole mass. There is a non-linear dependence of the Balmer line IC and BC luminosities with L$_{2-10keV}$ and L$_{5100}$, which suggests that a second-order factor such as the ILR and BLR covering factors affect the Balmer line component luminosities. The Balmer decrement is found to decrease from ~5 in the line core to ~2 in the extended wings, with mean decrements of 2.1 in BLR and 4.8 in ILR. This suggests different physical conditions in these regions. The [OIII] line is composed of a narrow core together with a blue-shifted component with average outflow velocity of $130^{+230}_{-80} km s^{-1}$. The total luminosity of [OIII] λ5007 well correlates with the hard X-ray luminosity.
Systematic Study of AGN Clumpy Tori with Broadband X-ray Spectroscopy: Updated Unified Picture of AGN Structure
我们提出了使用X射线cluttertorus模型对附近活动星系核（AGN）进行系统的宽带X射线光谱分析的结果（XCLUMPY; Tanimoto et al. 2019）。通过增加本文新分析的16个活动星系核，我们研究了Ichikawa et al.（2015）和García-Bernete et al.（2019）的28个活动星系核，包括未吸收和吸收的活动星系核。这是最大的样品，其X射线和红外光谱分别由cluplantorus模型XCLUMPY和CLUMPY（Nenkova等人，2008）进行分析。根据每个物体的X射线环面参数确定的爱丁顿比和环面覆盖因子之间的关系遵循Ricci等人（2017）基于统计分析发现的趋势。我们证实了Tanimoto等人（2020）的结果：（1）红外数据确定的环面角宽度大于X射线数据确定的环面角宽度;（2）在遮蔽活动星系核中，沿视线方向的氢柱密度与V波段消光比（$N_{\rm H}/A_{\rm V}$）与银河系的平均值相似。未遮蔽的活动星系核的视向$N_{\rm H}/A_{\rm V}$比明显小于银河系的视向比。我们的研究结果可以很好地解释了一个更新的统一的图片AGN结构，包括一个尘埃环，尘埃极地流出，和无尘气体，其中的倾斜度决定了X射线和光学分类和观测到的环面属性在X射线和红外波段。
