论文标题
XMM-Newton和Seyfert 1 AGN NGC 5940的Swift观察
XMM-Newton and Swift Observations of the Seyfert 1 AGN NGC 5940
论文作者
论文摘要
探测活性银河核（AGN）围绕积聚流的物理学对于理解其发射机制至关重要，并且能够约束周围不同区域的几何和变异性能。软X射线多余（通常在$ \ sim2 \，\ mathrm {kev} $下方观察到的超过主导X射线PowerLaw Continuum）是一个突出的功能，在1型Seyfert AGN中通常可以看到，因此很容易地提供了这些系统围绕这些系统的积分流动机制的有用诊断。 NGC 5940是Seyfert 1 AGN，它显示出强大的，突出的软X射线过剩$ \ sim2 \，\ Mathrm {kev} $，在其XMM-Newton和Swift观察中都可以看到。拟合数据的模型表明，这一特征可以通过电离部分覆盖，热组合和模糊反射模型来很好地解释。尽管其他模型不能用手头的数据决定性地排除，但是缺乏大量的宽铁$K_α$以及反射光谱仪（RGS）数据中的任何显着的发射/吸收线特征倾向于倾向于在NGC 5940中偏爱软X射线过量的热组合起源。
Probing the physics of the accretion flow around active galactic nuclei (AGN) is crucial to understanding their emission mechanisms as well as being able to constrain the geometrical and variability properties of the different regions around them. The soft X-ray excess -- usually observed below $\sim2\,\mathrm{keV}$ in excess of the dominant X-ray powerlaw continuum -- is one prominent feature that is commonly seen in type 1 Seyfert AGN and therefore readily provides a useful diagnostic of the accretion flow mechanism around these systems. NGC 5940 is a Seyfert 1 AGN which reveals strong, prominent soft X-ray excess below $\sim2\,\mathrm{keV}$ as seen in both its XMM-Newton and Swift observations. Model fit to the data revealed that this feature could be equally well explained by the ionised partial covering, the thermal Comptonisation and the blurred reflection models. Although the other models cannot be decisively ruled out with the data at hand, the lack of significant broad iron $K_α$ as well as any significant emission/absorption line features in the reflection grating spectrometer (RGS) data tend to favour the thermal Comptonisation origin for the soft X-ray excess in NGC 5940.
