XMM-牛顿明亮偶然巡天中AGN星群的X射线光谱特性
The X-ray spectral properties of the AGN population in the XMM-Newton bright serendipitous survey
摘要：
我们在这里提出了一个详细的X射线光谱分析的活动星系核属于XMM-牛顿明亮的调查（XBS），包括超过300个活动星系核的红移~ 2.4。我们进行了X射线分析以下两种不同的方法：通过单独分析每个活动星系核的X射线光谱，并通过构建不同类型的活动星系核的平均光谱。从单个的分析中，我们发现光谱指数和源的硬X射线光度之间似乎存在着反相关，使得高光度源（> 10 E44 erg/s）的平均光子指数明显比低光度源的平均光子指数平坦。我们还发现，本征柱密度分布同意活动星系核的统一计划，虽然发现了一些例外（3%的整个样本），这是更常见的光学分类2型活动星系核。我们还发现，活动星系核X射线谱中除了固有的吸收外，还有一个主要的偏离幂律形状的现象，即所谓的“软过剩”，它清楚地显示出未吸收和吸收活动星系核的不同特征，并可能是不同的起源。关于平均光谱的形状，我们发现，它是最好的再现由一个未吸收（吸收）的功率定律，一个狭窄的Fe Ka发射线和一个小（大）量的反射未吸收（吸收）源的组合。我们没有显着检测到任何相对论贡献的线发射，我们计算其等效宽度（EW）的上限为230 eV的3西格玛置信水平。最后，通过将1型活动星系核样本分为高光度和低光度源，我们略微检测到随着光度增加，窄Fe K α线EW和反射量减少，即“所谓的”岩泽-谷口效应。
英文摘要：
We present here a detailed X-ray spectral analysis of the AGN belonging to the XMM-Newton bright survey (XBS) that comprises more than 300 AGN up to redshift ~ 2.4. We performed an X-ray analysis following two different approaches: by analyzing individually each AGN X-ray spectrum and by constructing average spectra for different AGN types. From the individual analysis, we find that there seems to be an anti correlation between the spectral index and the sources' hard X-ray luminosity, such that the average photon index for the higher luminosity sources (> 10E44 erg/s) is significantly flatter than the average for the lower luminosity sources. We also find that the intrinsic column density distribution agrees with AGN unified schemes, although a number of exceptions are found (3% of the whole sample), which are much more common among optically classified type 2 AGN. We also find that the so-called "soft-excess", apart from the intrinsic absorption, constitutes the principal deviation from a power-law shape in AGN X-ray spectra and it clearly displays different characteristics, and likely a different origin, for unabsorbed and absorbed AGN. Regarding the shape of the average spectra, we find that it is best reproduced by a combination of an unabsorbed (absorbed) power law, a narrow Fe Kalpha emission line and a small (large) amount of reflection for unabsorbed (absorbed) sources. We do not significantly detect any relativistic contribution to the line emission and we compute an upper limit for its equivalent width (EW) of 230 eV at the 3 sigma confidence level. Finally, by dividing the type 1 AGN sample into high- and low-luminosity sources, we marginally detect a decrease in the narrow Fe Kalpha line EW and in the amount of reflection as the luminosity increases, the "so-called" Iwasawa-Taniguchi effect.
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