论文标题
裸露seyfert 1 Galaxy ESO 511-G030中反射特征起源的X射线光谱研究
An X-ray spectral study of the origin of reflection features in bare Seyfert 1 galaxy ESO 511--G030
论文作者
论文摘要
活跃银河核（AGN）的重新处理的X射线发射是研究超级质量黑洞（SMBHS）围绕物质的动力学和几何形状的重要诊断工具。我们介绍了Bare Seyfert 1 Galaxy，ESO〜511-G030的宽带（光到硬X射线），分别使用了2012年和2007年的XMM-Newton数据。 ESO〜511-G030的宽带光谱显示出一个紫外线凹凸，一个低于2 KEV的突出的软孔，相对较宽（$σ= 0.08-0.14 $ keV）Fe发射线在6.4 KeV和E> 10 KeV处的Compton Hump弱。 ESO〜511-G030中的软X射线过量可以被描述为磁盘种子光子的热填充（$ 0.40^{+0.40^{+0.02} _ { - 0.02} $ KEV），光学厚度（$τ= 12.7^{+0.5} _ {+0.5} _ { - 0.4} _ {-0.4} $ {$）和cor {$ compact（由于未截断，中度至高度离子的积聚磁盘的反射模糊。但是，对于模糊的反射，该模型需要对磁盘和电晕进行一些极端的配置。这两种型号都均均均均具有快速旋转的黑洞（$ a> 0.78 $）和紧凑的电晕，这表明宽Fe发射线的相对论起源。我们发现以$ \ sim 2-3 $ eV为$ \ sim的内部磁盘温度，该温度以sub-eDdington速率（$λ_{edd} = 0.004-0.008 $）来表征UV凹凸和SMBH积聚。
The reprocessed X-ray emission from Active Galactic Nuclei (AGN) is an important diagnostic tool to study the dynamics and geometry of the matter surrounding the supermassive black holes (SMBHs). We present a broadband (optical-UV to hard X-ray) spectral study of the bare Seyfert 1 galaxy, ESO~511--G030, using multi-epoch Suzaku and XMM-Newton data from 2012 and 2007 respectively. The broadband spectra of ESO~511--G030 exhibit a UV bump, a prominent soft-excess below 2 keV, a relatively broad ($σ=0.08 - 0.14$ keV) Fe emission line at 6.4 keV and a weak Compton hump at E > 10 keV. The soft X-ray excess in ESO~511--G030 can be described either as the thermal Comptonization of disk seed photons by a warm ($0.40^{+0.02}_{-0.02}$ keV), optically thick ($τ= 12.7^{+0.5}_{-0.4}$) and compact ($< 15 \rm r_{g}$) corona or as the blurred reflection from an untruncated and moderate to highly ionized accretion disk. However, for the blurred reflection, the model requires some extreme configuration of the disk and corona. Both these models prefer a rapidly spinning black hole ($a>0.78$) and a compact corona, indicating a relativistic origin of the broad Fe emission line. We found an inner disk temperature of $\sim 2-3$ eV that characterises the UV bump and the SMBH accretes at a sub-Eddington rate ($λ_{Edd} = 0.004-0.008$).
