The Variable Relativistic Outflow of IRAS 13224–3809
The Variable Relativistic Outflow of IRAS 13224–3809
复制标题
IRAS 13224–3809 的可变相对论流出
DOI：
10.3847/1538-4357/aae438
复制
发表时间：
2018
期刊：
影响因子：
--
通讯作者：
Manuel H. Cañas
中科院分区：
文献类型：
--
作者：
G. Chartas;Manuel H. Cañas
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。超快流出首先通过检测高蓝移吸收线推断，然后用主成分分析证实。报道的这种流出的两个特性不同于在其他具有超快流出的agn中通常检测到的特性。首先，流出速度在v = 0.236c±0.006c时没有变化。其次，高蓝移吸收线的等效宽度与该源的3-10 keV通量呈负相关。考虑到背景的影响，我们对IRAS 13224−3809的XMM-Newton观测结果进行了重新分析。我们还采用了一种不同的分析方法来结合光谱，并研究了流出物的性质随3-10 keV通量和时间的变化。我们证实了IRAS 13224−3809中存在超快外流；然而，我们发现帕克等人分析中使用的背景光谱在蓝移铁谱线附近的能量中占主导地位。通过减少源提取区域以提高信噪比，我们发现了比以前报道的更大的流出速度，并且发现流出速度在~ 0.2c到~ 0.3c之间变化，并且随着3-10 keV通量的增加而增加。通过优化源提取区域，减小背景光谱后，铁谱线等效宽度与3-10 keV通量之间的不相关关系消失。
The discovery of an ultrafast outflow has been reported in the z = 0.0658 narrow-line Seyfert galaxy IRAS 13224−3809. The ultrafast outflow was first inferred through the detection of highly blueshifted absorption lines and then confirmed with a principal component analysis. Two of the reported properties of this outflow differed from those typically detected in other AGNs 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 anticorrelated with the 3–10 keV flux of this source. We present a reanalysis 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 anticorrelation 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.
DOI：
10.1046/j.1365-8711.2003.07006.x
发表时间：
2003-03
影响因子：
4.8
作者：
K. Pounds;J. Reeves;A. King;K. Page;P. O’Brien;M. W. D. O. PhysicsAstronomy;U. Leicester;Laboratory for Multiwavelength Astrophysics;Nasa Gsfc
通讯作者：
K. Pounds;J. Reeves;A. King;K. Page;P. O’Brien;M. W. D. O. PhysicsAstronomy;U. Leicester;Laboratory for Multiwavelength Astrophysics;Nasa Gsfc
影响因子：
64.8
作者：
F. Tombesi;M. Meléndez;S. Veilleux;J. Reeves;E. González-Alfonso;C. S. R. Nasagsfccresst;U. Maryland-U.-Mary
通讯作者：
F. Tombesi;M. Meléndez;S. Veilleux;J. Reeves;E. González-Alfonso;C. S. R. Nasagsfccresst;U. Maryland-U.-Mary
变化的活跃星系核的时间变化的辐射磁流体动力学模拟
DOI：
--
发表时间：
2020
期刊：
影响因子：
--
作者：
Taichi Igarashi;Y. Kato;H.R. Takahashi;K. Ohsuga;R. Matumoto
通讯作者：
R. Matumoto