论文标题
重新观察NLS1 Galaxy RE J1034+396。 ii。关于软X射线过剩，QPO和与GRS 1915+105的类比的新见解
Re-observing the NLS1 Galaxy RE J1034+396. II. New Insights on the Soft X-ray Excess, QPO and the Analogy with GRS 1915+105
论文作者
论文摘要
活跃的银河核（AGN）RE J1034+396显示到迄今为止检测到的最显着的X射线准周期振荡（QPO）。我们对最近同时的XMM-Newton，Nustar和Swift观察进行了详细的频谱定时分析。我们介绍了QPO频率，RMS，相干性和相位滞后的能量依赖性，并将它们与时间平均光谱进行建模。我们的研究表明，需要四个组件才能拟合所有光谱。这些组件包括一个内盘组件（DISKBB），两个温暖的电晕组件（COMPTT-1和COMPTT-2）和一个热的电晕组件（NTHCOMP）。我们发现DISKBB，COMPTT-2（更热但发光的分量更低）和NTHCOMP都包含QPO信号，而COMPTT-1仅显示随机变化。通过拟合滞后频谱，我们发现diskbb中的QPO导致COMPTT-2降低679 s，而Comptt-2则导致NTHCOMP 180 s。通过仅改变正常化，这些组件也可以与从QPO存在且不存在的先前观察结果获得的时间平均和可变性光谱产生良好的拟合。我们的多波长研究表明，QPO的可检测性不取决于同时的质量积聚率。我们没有检测到明显的铁Kα发射线或任何显着的反射驼峰。最后，我们表明，在最新观察结果中的RMS和滞后光谱与在微观Quasar GRS 1915+105中观察到的67 Hz QPO非常相似。这些新结果支持这两个来源之间的物理类比。我们推测两个来源中的QPO都是由于内盘垂直结构的扩展/收缩所致。
The active galactic nucleus (AGN) RE J1034+396 displays the most significant X-ray Quasi-Periodic Oscillation (QPO) detected so far. We perform a detailed spectral-timing analysis of our recent simultaneous XMM-Newton, NuSTAR and Swift observations. We present the energy dependence of the QPO's frequency, rms, coherence and phase lag, and model them together with the time-averaged spectra. Our study shows that four components are required to fit all the spectra. These components include an inner disc component (diskbb), two warm corona components (CompTT-1 and CompTT-2), and a hot corona component (nthComp). We find that diskbb, CompTT-2 (the hotter but less luminous component) and nthComp all contain the QPO signal, while CompTT-1 only exhibits stochastic variability. By fitting the lag spectrum, we find that the QPO in diskbb leads CompTT-2 by 679 s, and CompTT-2 leads nthComp by 180 s. By only varying the normalizations, these components can also produce good fits to the time-averaged and variability spectra obtained from previous observations when QPOs were present and absent. Our multi-wavelength study shows that the detectability of the QPO does not depend on the contemporaneous mass accretion rate. We do not detect a significant Iron Kα emission line, or any significant reflection hump. Finally, we show that the rms and lag spectra in the latest observation are very similar to the 67 Hz QPO observed in the micro-quasar GRS 1915+105. These new results support the physical analogy between these two sources. We speculate that the QPO in both sources is due to the expansion/contraction of the vertical structure in the inner disc.
