超大质量黑洞吸积盘中X射线谱线的研究是研究吸积流物理和几何的重要手段之一，同时也为黑洞的自旋提供了理论上的观测约束。[...]我们的目标是确定这种相对论性再处理功能的强度的最终物理驱动程序。我们首先将目前研究的塞弗特星系的硬X射线通量限制样本（FERO，de la Calle Perez et al. 2010）扩展到柱密度N_H=6x10^23 atoms/cm/cm的遮蔽天体。我们验证，没有线属性依赖于活动星系核的光学分类，预期从塞弗特统一方案。也没有相关的吸积盘的倾角，从正式拟合的线配置文件，和光学类型或宿主星系的方位角，这表明吸积盘和宿主星系平面的最里面的区域不对齐。[...].数据对线发射盘的详细电离状态不够敏感。然而，缺乏依赖性的线EW上的光度或静止帧质心能量排除了光盘电离在EW的动态范围在塞弗茨起着重要的作用。相对论性加宽的K-α铁线EW的动力学范围在附近的Seyferts似乎主要是由最里面的吸积流的属性。我们讨论了几种机制（光盘电离，光盘截断，由于轻度相对论外流电晕畸变），可以解释这一点。[...]观测数据仍然不矛盾的情况下调用不同的机制的光谱复杂性周围的铁线，最值得注意的是“部分覆盖”吸收的情况。（节略）。
英文摘要：
Spectroscopy of X-ray emission lines emitted in accretion discs around supermassive black holes is one of the most powerful probes of the accretion flow physics and geometry, while also providing in principle observational constraints on the black hole spin.[...] We aim at determining the ultimate physical driver of the strength of this relativistic reprocessing feature. We first extend the hard X-ray flux-limited sample of Seyfert galaxies studied so far (FERO, de la Calle Perez et al. 2010) to obscured objects up to a column density N_H=6x10^23 atoms/cm/cm. We verify that none of the line properties depends on the AGN optical classification, as expected from the Seyfert unification scenarios. There is also no correlation between the accretion disc inclination, as derived from formal fits of the line profiles, and the optical type or host galaxy aspect angle, suggesting that the innermost regions of the accretion disc and the host galaxy plane are not aligned. [...]. Data are not sensitive enough to the detailed ionisation state of the line-emitting disc. However, the lack of dependency of the line EW on either the luminosity or the rest-frame centroid energy rules out that disc ionisation plays an important role on the EW dynamical range in Seyferts. The dynamical range of the relativistically broadened K-alpha iron line EW in nearby Seyferts appears to be mainly determined by the properties of the innermost accretion flow. We discuss several mechanisms (disc ionisation, disc truncation, aberration due to a mildly relativistic outflowing corona) which can explain this. [...] Observational data are still not in contradiction with scenarios invoking different mechanisms for the spectral complexity around the iron line, most notably the "partial covering" absorption scenario. (abridged).
High-resolution X-ray spectroscopy of the low and high states of the Seyfert 1 galaxy NGC 4051 with Chandra LETGS
方法.本文分析了Chandra低能透射光栅光谱仪的两个观测结果。我们研究了光谱响应突然通量减少的一个因素，这发生在第二次观察。结果我们检测到一个高度电离的吸收组件的流出速度为-4670公里/秒，在塞弗特1星系中观察到的最高流出速度的组件之一。该光谱包含一个相对论O VIII Ly α线，和四个吸收组件跨越范围的电离参数XI在0.07和3.19之间。在低态出现了产生CVI和CV辐射复合连续谱的发射分量。黑体温度随着第二次观测中观测到的通量的下降而下降。结论.对于所有的吸收器组件，我们排除了电离参数线性响应通量的减少了5倍。吸收体的可变性表明，四个检测到的组分中至少有三个位于0.02-1 pc的范围内。删节
