RE J1034+396 displays the so far detected most significant X-ray Quasi-Periodic Oscillation (QPO) in AGN. We perform a detailed spectral-timing analysis on the data using recent simultaneous XMM-Newton, NuSTAR and Swift observations. We present the detailed energy dependence of the QPO's frequency, rms, coherence and phase lag. We construct various frequency-resolved variability spectra, which are modelled together with the time-averaged spectra. Our study shows that four components are required to fit all the spectra, including an inner disc component (diskbb), two warm corona components (CompTT-1 and CompTT-2) and a hot corona component (nthComp). An important discovery is that within the two warm corona components, CompTT-2 (the hotter, less luminous component) contains the QPO signal, while the stochastic variability is concentrated in CompTT-1. These components also allow us to fit the lag-energy spectra, as well as being able to describe the previous observation of a strong QPO in 2007, and the absent QPO observations, by varying only the relative normalizations of these components. Our multi-wavelength study shows that the QPO's detectability does not depend on the contemporaneous mass accretion rate through the outer disc as estimated from the UV flux. We do not detect a significant Iron K$\alpha$ line, nor any significant reflection component hump. Finally, we show that the rms and lag spectra of RE J1034+396 in the recent observation are very similar to the 67 Hz QPO in the micro-quasar GRS 1915+105. These new results reinforce the physical analogy between the two sources. We speculate that the QPO in both sources is due to expansion/contraction of the inner disc vertical structure.

中文翻译：

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重新观察 NLS1 Galaxy RE J1034+396。二、关于软 X 射线过剩、QPO 和 GRS 1915+105 类比的新见解

RE J1034+396 显示了迄今为止在 AGN 中检测到的最重要的 X 射线准周期性振荡 (QPO)。我们使用最近同时进行的 XMM-Newton、NuSTAR 和 Swift 观测对数据进行了详细的光谱时序分析。我们展示了 QPO 的频率、均方根值、相干性和相位滞后的详细能量依赖性。我们构建了各种频率分辨变异谱，这些谱与时间平均谱一起建模。我们的研究表明，需要四种成分来拟合所有光谱，包括内盘成分 (diskbb)、两种暖电晕成分（CompTT-1 和 CompTT-2）和热电晕成分 (nthComp)。一个重要的发现是，在两个温暖的日冕成分中，CompTT-2（更热、亮度更低的成分）包含 QPO 信号，而随机变异性集中在 CompTT-1 中。这些分量还使我们能够拟合滞后能谱，并能够通过仅改变这些分量的相对归一化来描述 2007 年强 QPO 的先前观察结果和不存在的 QPO 观察结果。我们的多波长研究表明，QPO 的可探测性不依赖于通过外部圆盘的同期质量吸积率，这是根据紫外线通量估计的。我们没有检测到明显的 Iron K$\alpha$ 线，也没有检测到任何明显的反射分量驼峰。最后，我们表明最近观测中 RE J1034+396 的 rms 和滞后谱与微类星体 GRS 1915+105 中的 67 Hz QPO 非常相似。这些新结果加强了两个来源之间的物理类比。