极端NLS1 IRAS13224-3809中的相对论圆盘反射
Relativistic disc reflection in the extreme NLS1 IRAS13224-3809
摘要：
我们提出了一个光谱变率的研究XMM-牛顿和朱雀观测的最极端的窄线塞弗特1星系，IRAS 13224 -3809。X射线光谱的特征在于两个主要的独特特征，i）在低于约1.3keV时具有陡峭上升的强软过剩，以及ii）在高于8.2keV时通量的深下降。在这里，我们专注于一个基于反射的解释，解释这两个功能，以及大软过剩，在部分电离反射关闭内吸积盘。结果表明，上述两种特殊的光谱特征可以用两条相对论性的FeK和FeL发射线来再现。这些线产生于内部吸积盘中，并独立地产生一致的盘参数。我们认为，高的L/K强度比是大致一致的期望从电离吸积盘反射，表明它们属于一个单一的电离反射组件。光谱形状，X射线通量和变化特性在XMM-牛顿和朱雀观测中非常相似，间隔约5年。整体的X射线光谱和可变性可以用一个简单的两组分模型来描述，该模型包括一个陡峭的幂律连续体加上其电离反射的内部吸积盘。在这个模型中，需要一个快速旋转的克尔黑洞和一个陡峭的发射率轮廓来描述数据。在IRAS 13224-3809中同时检测到宽相对论性Fe L和K线，这是继另一个极端NLS 1星系1H 0707 -495之后的结果。尽管IRAS 13224 -3809的数据质量不允许我们排除1H 0707 -495中的竞争模型，但我们在此表明，我们基于反射的解释以自洽的方式描述了可用数据，并指出IRAS 13224 -3809在光谱和变异性方面与1H 0707 -495非常接近。
英文摘要：
We present a spectral variability study of the XMM-Newton and Suzaku observations of one of the most extreme Narrow Line Seyfert 1 galaxies, IRAS13224-3809. The X-ray spectrum is characterized by two main peculiar features, i) a strong soft excess with a steep rise below about 1.3 keV and ii) a deep drop in flux above 8.2 keV. We focus here on a reflection-based interpretation which interprets both features, as well as the large soft excess, in terms of partially ionized reflection off the inner accretion disc. We show that the two peculiar spectral features mentioned above can be reproduced by two relativistic emission lines due to Fe K and Fe L. The lines are produced in the inner accretion disc and independently yield consistent disc parameters. We argue that the high L/K intensity ratio is broadly consistent with expectations from an ionized accretion disc reflection, indicating that they belong to a single ionized reflection component. The spectral shape, X-ray flux, and variability properties are very similar in the XMM-Newton and Suzaku observations, performed about 5 years apart. The overall X-ray spectrum and variability can be described by a simple two-component model comprising a steep power law continuum plus its ionised reflection off the inner accretion disc. In this model, a rapidly rotating Kerr black hole and a steep emissivity profile are required to describe the data. The simultaneous detection of broad relativistic Fe L and K lines in IRAS 13224-3809 follows that in another extreme NLS1 galaxy, 1H0707-495. Although the data quality for IRAS13224-3809 does not allow us to rule out competing models as in 1H0707-495, we show here that our reflection-based interpretation describes in a self-consistent manner the available data and points towards IRAS13224-3809 being a very close relative of 1H0707-495 in terms of both spectral and variability properties.
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