We present a multi-waveband analysis of a 126 galaxy sub-sample of the 12 micron galaxy sample (12MGS), for which we have carried out a detailed X-ray spectral analysis of in a previous paper. We present optical activity classes and we characterise these by their X-ray, 12 um and [OIII] luminosities and by their X-ray spectral properties. Our most interesting results are: Seyfert (Sy) 1s and Sy 2s show significantly different LX distributions from each other; Sy 2s with a detection of an HBLR show a significantly higher LX than those without a detection; Sy 1s also present a significantly different L(12um) distribution from both Sy1.2-1.9s and Sy 2s; the Sy 2 fraction decreases towards high LX; X-ray indications of AGN power agree well with the optical classifications; There is X-ray evidence for the presence of an AGN in 17% of HII/AGN composites and 40% of LINERs; we advocate the use of a LX >10^41 erg/s in the X-ray selection of AGN, which gives a contamination rate of only 3% from star-forming galaxies; Sy 1s and Sy 2 have the same intrinsic Γ; in 24% of cases the absorption measured in X-rays does not correspond directly with that implied in the optical band from the visibility of the BLRs; the obscured fraction in AGN is a strong function of LX peaking at 10^42 erg/s; The average obscured and Compton thick fractions for this sample are 62\pm5% and 20\pm4% respectively, which are higher than hard X-ray and optically selected samples; we assess the use of the T ratio (FX/F[OIII]) for selecting Compton thick candidates. We conclude here that this quantity can often be unreliable due uncertainties in the extinction corrections to the [OIII] flux. These results have important impacts on AGN selection and unification and the results from the 12MGS are particularly useful as a local analogue to z=1 24 um samples.
A Sharper View of the X-ray Spectrum of MCG--6-30-15 with XRISM, XMM-Newton and NuSTAR
The Ohio State University（俄亥俄州立大学）；University of Maryland, College Park（马里兰大学帕克分校）；NASA / Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；Center for Research and Exploration in Space Science and Technology, NASA / GSFC (CRESST II)（NASA/GSFC空间科学与技术研究探索中心（CRESST II））；University of Chicago（芝加哥大学）；Institute of Astronomy, Cambridge University（剑桥大学天文研究所）；California Institute of Technology（加州理工学院）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究研究所）；University of Teacher Education Fukuoka（福冈教育大学）；Tohoku University（东北大学）；Technion（以色列理工学院）；University of Maryland, Baltimore County (UMBC)（马里兰大学巴尔的摩县分校）；European Space Agency (ESA), European Space Research and Technology Centre (ESTEC)（欧洲空间局欧洲空间研究与技术中心）；SRON Netherlands Institute for Space Research（荷兰空间研究研究所）；University of Leiden（莱顿大学）；University of Miyazaki（宫崎大学）
1 ES 1927+654是一个活动星系核（AGN），似乎与统一模型相悖。它具有2型光谱，但几乎没有X射线遮蔽。利用2011年获得的XMM-Newton和Suzaku观测数据研究了1 ES 1927+654的X射线性质。利用XMM-Newton同步光学-X射线数据得到的光谱能量分布表明活动星系核具有典型的爱丁顿比（L/LEdd = 0.014-0.11）。X射线光谱和快速的变化是一致的起源于一个标准的吸积盘周围的日冕。部分覆盖模型可以描述的X射线数据，但是，窄Fe Ka发射线预测标准光电吸收没有检测到。电离的部分覆盖也有利于高速外流（v ~ 0.3c），这要求风的动力学光度大于活动星系核辐射光度的30%。这样的值并不罕见，但对于1 ES 1927+654，它需要风非常接近黑洞（~ 10 Rg）。模糊反射模型也可以很好地描述1 ES 1927+654的光谱和时间特性，如果活动星系核被视为近侧，这意味着一个内部吸积盘必须存在。高倾角是有趣的，因为它表明1 ES 1927+654可以像塞弗特2一样定向，与它的光学分类一致，但通过一个脆弱的环面观察。
The narrow Fe K$α$ line and the molecular torus in active galactic nuclei - an IR/X-ray view
铁K $α$的窄组分在活动星系核（AGN）的X射线谱中几乎是普遍存在的特征，并且被认为起源于中性物质，可能位于分子环中。这将意味着铁K $α$等效宽度（EW）和环面的物理性质之间的紧密联系。在最近的一项工作中，我们已经表明，环面的覆盖因子随着光度的减少，正如光度依赖的统一模型所预期的那样，将能够解释Fe K $α$ EW随着光度的减少（即，X射线鲍德温效应）。活动星系核中红外光谱研究的最新进展使得人们可以利用星团环面模型来推导活动星系核的重要参数，如覆盖因子（$f_{\rm\,obs}$）和赤道柱密度（$N_{\rm\,H}^{\rm\,T}$）。利用对24个Ⅰ型活动星系核样品的XMM Newton/EPIC观测，研究了最近MIR工作获得的环面物理参数与Fe K $α$线性质之间的关系.我们采取的倾斜角，光子指数，赤道柱密度，半开角的环面考虑使用物理环面模型的X射线再处理辐射的Fe K $α$ EW的值。我们发现，铁K $α$ EW和$f_{\rm\,obs}$之间的关系显示出与预期值一致的斜率，尽管具有较低的统计显著性。当比较Fe K $α$ EW和$N_{\rm\,H}^{\rm\,T}$时，也发现了与理论预测一致的趋势。我们的工作似乎证实，大量的窄Fe K $α$线是由负责MIR发射的相同材料产生的。
