IRAS 13224-3809的可变相对论流出
The Variable Relativistic Outflow of IRAS 13224-3809
摘要：
据报道，在z=0.0658窄线塞弗特星系IRAS 13224-3809中发现了超快外流（Parker et al. 2017 a）。首先通过检测高度蓝移的吸收线推断出超快流出（Parker等人，2017 a），然后用主成分分析（PCA）证实（Parker等人，2017 b）。这流出的两个报告的属性不同于那些通常在其他活动星系核与超快流出检测。首先，发现流出速度不随v=0.236c +/- 0.006c而变化。第二，高度蓝移的吸收线的等效宽度被报道与该源的3-10 keV通量反相关。本文对IRAS 13224-3809的XMM-牛顿观测进行了考虑背景影响的再分析。我们还进行了不同的分析方法，结合光谱和研究的流出作为3-10千电子伏通量和时间的函数的属性的变化。我们证实了IRAS 13224-3809中存在超快外流，然而，我们发现Parker等人分析中使用的背景光谱主导了蓝移铁线附近能量的源光谱。通过减小源提取区域以提高信噪比，我们发现流出速度比以前报道的要大，并且发现流出速度在~0.2c ~0.3c之间变化，并且随着3-10~keV通量的增加而增加。通过优化源引出区，降低了背景光谱，消除了铁谱线等效宽度与3-10 keV通量之间的反相关性。
英文摘要：
The discovery of an ultrafast outflow has been reported in the z=0.0658 narrow line Seyfert galaxy IRAS 13224-3809 (Parker et al. 2017a). The ultrafast outflow was first inferred through the detection of highly blueshifted absorption lines (Parker et al. 2017a) and then confirmed with a principal component analysis (PCA) (Parker et al. 2017b). Two of the reported properties of this outflow differed from those typically detected in other AGN with ultrafast outflows. First, the outflow velocity was found not to vary with v=0.236c +/- 0.006c. Second, the equivalent width of the highly blueshifted absorption line was reported to be anti-correlated with the 3-10 keV flux of this source. We present a re-analysis of the XMM-Newton observations of IRAS 13224-3809 considering the influence of background. We also undertook a different analysis approach in combining the spectra and investigated the change of the properties of the outflow as a function of 3-10 keV flux and time. We confirm the presence of an ultrafast outflow in IRAS 13224-3809, however, we find that the background spectra used in the Parker et al. analyses dominate the source spectra for energies near the blueshifted iron lines. By reducing the source extraction regions to improve the signal-to-noise ratio we discover larger than previously reported outflow velocities and find that the outflow velocity varies from ~0.2c to ~0.3c and increases with 3-10~keV flux. The previously reported anti-correlation between equivalent width of the iron line and 3-10 keV flux disappears when the background spectra are reduced by optimizing the source extraction regions.
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