The 1.5 Ms observing campaign on IRAS 13224-3809 - I. X-ray spectral analysis
The 1.5 Ms observing campaign on IRAS 13224-3809 - I. X-ray spectral analysis
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DOI：
10.1093/mnras/sty836
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发表时间：
2018-04
影响因子：
4.8
通讯作者：
Jiachen Jiang;M. L. Parker;M. L. Parker;A. Fabian;W. Alston;D. Buisson;E. Cackett;C. Chiang;T. Dauser;L. Gallo;Javier A. García;F. Harrison;A. Lohfink;B. Marco;E. Kara;Jonathan M. Miller;G. Miniutti;C. Pinto;D. Walton;D. Wilkins
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作者：
Jiachen Jiang;M. L. Parker;M. L. Parker;A. Fabian;W. Alston;D. Buisson;E. Cackett;C. Chiang;T. Dauser;L. Gallo;Javier A. García;F. Harrison;A. Lohfink;B. Marco;E. Kara;Jonathan M. Miller;G. Miniutti;C. Pinto;D. Walton;D. Wilkins
我们提出了一个详细的光谱分析，最近1.5兆XMM-牛顿观测活动的窄线塞弗特1星系IRAS 13224 - 3809，同时采取了500 ks的努斯塔数据。X射线光变曲线显示了三个通量峰值，记录了活动期间最小通量的100倍，以及以千秒为时间尺度的快速变化。的光谱是很好的拟合与一个主要的幂律连续，两个相对论模糊的反射组件从内部吸积盘具有非常高的铁丰度，和一个简单的黑体形状的模型剩余的软过剩。光谱的变化主要是由幂律连续从日冕区域内的几个引力半径的黑洞。此外，蓝移的Ne X，Mg XII，Si XIV和S XVI吸收线被确定在堆叠的低通量光谱，确认存在高度电离的流出速度高达v = 0.267和0.225 c。我们用xstar模型拟合了吸收特征，发现在整个观测过程中有一个相对恒定的速度流出。最后，我们通过使用扩展反射模型relxillD成功拟合软过剩来替换bbody和超太阳丰度反射模型，该模型允许比标准relxill模型更高的密度。这使圆盘电子密度n_e > 10^（18.7）cm^（-3），并使铁丰度从Z_（Fe）= 24^（+3）_（-4）Z_d（n-e = 10^（15）cm^（-3））降低到Z_（Fe）= 6.6^（+0.8）_（-2.1）Z_d。
We present a detailed spectral analysis of the recent 1.5 Ms XMM–Newton observing campaign on the narrow-line Seyfert 1 galaxy IRAS 13224−3809, taken simultaneously with 500 ks of NuSTAR data. The X-ray light curve shows three flux peaks, registering at about 100 times the minimum flux seen during the campaign, and rapid variability with a time-scale of kiloseconds. The spectra are well fit with a primary power-law continuum, two relativistic-blurred reflection components from the inner accretion disc with very high iron abundance, and a simple blackbody-shaped model for the remaining soft excess. The spectral variability is dominated by the power-law continuum from a corona region within a few gravitational radii from the black hole. Additionally, blueshifted Ne X, Mg XII, Si XIV, and S XVI absorption lines are identified in the stacked low-flux spectrum, confirming the presence of a highly ionized outflow with velocity up to v = 0.267 and 0.225 c. We fit the absorption features with xstar models and find a relatively constant velocity outflow through the whole observation. Finally, we replace the bbody and supersolar abundance reflection models by fitting the soft excess successfully with the extended reflection model relxillD, which allows for higher densities than the standard relxill model. This returns a disc electron density n_e > 10^(18.7) cm^(−3) and lowers the iron abundance from Z_(Fe) = 24^(+3)_(−4)Z_⊙ with n-e = 10^(15) cm^(-3) to Z_(Fe) = 6.6^(+0.8)_(-2.1)Z_⊙.