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深钱德拉场AGN X射线谱的平均

Averaging the AGN X-ray spectra from deep Chandra fields

S. Falocco, F. J. Carrera, A. Corral, E. Laird, K. Nandra, X. Barcons, M. J. Page, J. Digby-North

备注：
17 pages, 23 figures, accepted for publication in Astronomy & Astrophysics. Replacements in the bibliography: Iwasawa K., Mainieri V., Brusa M., et al., 2011, arXiv:1111.2447v1 (previously: Iwasawa et al 2011, in preparation); Mateos S., Carrera F.J., Page M.J., et al., 2010, \aap, 510, A35 (previously: Mateos S., Warwick R.S., Carrera F.J., et al., 2008, \aap, 492, 51)
发表信息：
A&A 538, A83 (2012)
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摘要：

活动星系核（AGN）的X射线谱带有来自中心区域的辐射特征，靠近超大质量黑洞（SMBH）。因此，研究深X射线谱是研究其发射源的有力工具。活动星系核的X射线谱中最常观测到的发射线是Fe K。它是已知的，它可以扩大和变形的相对论效应，如果发射足够接近中央SMBH。在最近对活动星系核样品X射线谱的统计研究中，发现窄Fe谱线普遍存在，而宽Fe谱线是否普遍存在还不确定。本文介绍了在深钱德拉场中活动星系核平均X射线谱中Fe线特征的研究结果。活动星系核的平均光谱是使用来自AEGIS、Chandra Deep Field North和Chandra Deep Field South巡天的200多个净计数的Chandra光谱计算的。样品跨越了更广泛的X射线光度比其他样品研究堆叠方法高达z=3.5。我们使用我们自己的平均方法分析了该样品的平均光谱，并将结果与广泛的模拟进行了比较。定义在当地吸收体，光度和z的列密度的子样本也进行了研究。我们发现，在我们所有的样品和几乎所有的子样品，我们构建了一个非常显着的铁线与窄的配置文件。在整个样品的平均光谱中估计的窄线的等效宽度（EW）为74eV。在AGN子样品中检测到宽线分量，其L<1.431E44cgs，z<0.76，EW= 108eV。结果表明，在z= 3.5之前，活动星系核的X射线谱中普遍存在Fe的窄谱线，而在低亮度、低z的活动星系核的X射线谱中，宽谱线分量是重要的。

英文摘要：

The X-ray spectra of Active Galactic Nuclei (AGN) carry the signatures of the emission from the central region, close to the Super Massive Black Hole (SMBH). For this reason, the study of deep X-ray spectra is a powerful instrument to investigate the origin of their emission. The emission line most often observed in the X-ray spectra of AGN is Fe K. It is known that it can be broadened and deformed by relativistic effects if emitted close enough to the central SMBH. In recent statistical studies of the X-ray spectra of AGN samples, it is found that a narrow Fe line is ubiquitous, while whether the broad features are as common is still uncertain. We present here the results of an investigation on the characteristics of the Fe line in the average X-ray spectra of AGN in deep Chandra fields. The average spectrum of the AGN is computed using Chandra spectra with more than 200 net counts from the AEGIS, Chandra Deep Field North and Chandra Deep Field South surveys. The sample spans a broader range of X-ray luminosities than other samples studied with stacking methods up to z=3.5. We analyze the average spectra of this sample using our own averaging method, checking the results against extensive simulations. Subsamples defined in terms of column density of the local absorber, luminosity and z are also investigated. We found a very significant Fe line with a narrow profile in all our samples and in almost all the subsamples that we constructed. The equivalent width (EW) of the narrow line estimated in the average spectrum of the full sample is 74 eV. The broad line component is significantly detected in the subsample of AGN with L<1.43 1E44 cgs and z<0.76, with EW=108 eV. We concluded that the narrow Fe line is an ubiquitous feature of the X-ray spectra of the AGN up to z=3.5.The broad line component is significant in the X-ray spectra of the AGN with low luminosity and low z.

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