Complex X-Ray Absorption and the Fe Kα Profile in NGC 3516
Complex X-Ray Absorption and the Fe Kα Profile in NGC 3516
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NGC 3516 中的复杂 X 射线吸收和 Fe Kα 分布
DOI：
10.1086/425961
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
M. Bottorff
中科院分区：
文献类型：
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作者：
T. Turner;S. Kraemer;I. George;J. Reeves;M. Bottorff
我们提供了 2001 年 4 月和 11 月期间对 Seyfert 1 星系 NGC 3516 进行钱德拉 (Chandra)、XMM-牛顿 (XMM-Newton) 和 BeppoSAX 同时观测的数据。我们研究了观察到的非常平坦的 X 射线光谱的性质。钱德拉光栅数据显示 X 射线吸收线的存在，揭示了吸收气体的两种不同成分，一种与我们之前的 UV/X 射线吸收剂模型一致，而另一种以约 1100 km s-1 的速度流出，具有更大的柱密度和更高的电离度。 2001 年 4 月期间用 XMM-Newton 观测到的 X 射线连续谱的宽带光谱特征揭示了第三吸收层的存在，该吸收层由一个非常大的高度电离气体柱（约 2.5 × 1023 cm-2）组成，覆盖率约为 50%。这种低覆盖率表明吸收体位于 X 射线源的几光日内和/或具有丝状结构。有趣的是，这些吸收器彼此之间并不处于热平衡。这两种新成分的电离度太高，无法进行辐射加速，我们认为这是流出物磁流体起源的证据。将我们的模型应用于 11 月的数据集，我们可以主要通过吸收体电离态的下降来解释光谱变化，正如连续通量变化所预期的那样。当考虑到这种复杂的吸收时，我们发现潜在的连续体是 Seyfert 1 星系的典型特征。归因于高柱吸收体的光谱曲率反过来又减少了对吸积盘的通量和任何宽铁发射线范围的估计。
We present data from simultaneous Chandra, XMM-Newton, and BeppoSAX observations of the Seyfert 1 galaxy NGC 3516, taken during 2001 April and November. We have investigated the nature of the very flat observed X-ray spectrum. Chandra grating data show the presence of X-ray absorption lines, revealing two distinct components of the absorbing gas, one that is consistent with our previous model of a UV/X-ray absorber while the other, which is outflowing at a velocity of ~1100 km s-1, has a larger column density and is much more highly ionized. The broadband spectral characteristics of the X-ray continuum observed with XMM-Newton during 2001 April reveal the presence of a third layer of absorption consisting of a very large column (≈2.5 × 1023 cm-2) of highly ionized gas with a covering fraction ~50%. This low covering fraction suggests that the absorber lies within a few light days of the X-ray source and/or is filamentary in structure. Interestingly, these absorbers are not in thermal equilibrium with one another. The two new components are too highly ionized to be radiatively accelerated, which we suggest is evidence for a hydromagnetic origin for the outflow. Applying our model to the November data set, we can account for the spectral variability primarily by a drop in the ionization states of the absorbers, as expected by the change in the continuum flux. When this complex absorption is accounted for, we find the underlying continuum to be typical of Seyfert 1 galaxies. The spectral curvature attributed to the high column absorber in turn reduces estimates of the flux and the extent of any broad Fe emission line from the accretion disk.