AI 中文总结
本研究通过结合XMM-Newton和XRISM数据，揭示了Mrk 766中动态电离吸收体、宽Fe Kα发射线及紫外滞后，描绘了高吸积NLSy1系统的吸积盘-冕连接。
AI 中文摘要
我们通过对存档的跨越近二十年的\textit{XMM-Newton}观测以及在其性能验证阶段获得的\textit{XRISM}观测进行结合，对窄线 Seyfert 1 (NLSy1) 星系 Mrk~766 进行了多历元、主要为X射线波段的研究。我们分析了来自RGS和EPIC-pn数据的软X射线光谱中的吸收和发射特征，揭示了一个分层的多相可能电离吸收体，其柱密度在约1天的时间尺度上发生变化。覆盖分数与连续谱通量呈正相关，但在各历元之间存在显著的内在离散。Mrk~766 表现出多成分的Fe K$\alpha$发射线，这是通过对\textit{XRISM}数据的拟合揭示的。一个由环面和一个宽\textit{diskline}成分组成的准唯象模型区分了这两个成分，并将潜在宽发射线盘子结构的内半径限制在$R_{in}=40-60\\,r_{\rm g}$之间。对跨越\textit{XMM-Newton}观测的多个历元的Fe K$\alpha$复合体的分析表明，宽成分紧密跟踪连续谱通量，并有效反映了相对于连续谱的趋势。窄成分与一个遥远的发射体（可能是环面）一致。与\textit{Swift}-XRT和UVOT的准同步监测进一步表明，紫外发射滞后于X射线$5.9^{+4.1}_{-5.7}$小时，这与冕X射线波动的盘再处理一致，并对应于高达$10^{3}\\,r_{\rm g}$的光传播距离。总的来说，我们的分析描绘了这个高吸积率NLSy1系统中动态演化的吸收体、铁线发射体和吸积盘的范围。
英文摘要
We present a multi-epoch, primarily X-ray study of the narrow-line Seyfert 1 (NLSy1) galaxy Mrk~766 by combining archival \textit{XMM-Newton} observations spanning nearly two decades together with a \textit{XRISM} observation obtained during its Performance Verification Phase. We analyzed the absorption and emission features in the soft X-ray spectra from RGS and EPIC-pn data, revealing a stratified multi-phase potentially ionised absorber with a column density varying at a timescale of $\sim$1 day. The covering fraction shows positive correlation with the continuum flux, however with significant intrinsic scatter, between the epochs. Mrk~766 exhibits a multi-component Fe\,K$α$ emission line as revealed by fits to the \textit{XRISM} data. A quasi-phenomenological model comprising a torus and a broad \textit{diskline} component distinguishes the two components and constrains the inner radius of the potential broad line emitting disk substructure between $R_{in}=40-60\,r_{\rm g}$. Analysis of multiple epochs of the Fe K$α$ complex across \textit{XMM-Newton} observations reveals that the broad component tracks the continuum flux closely and effectively reflects the trend with respect to the continuum. The narrow component is consistent with a distant emitter, potentially the torus. Quasi-simultaneous monitoring with \textit{Swift}-XRT and UVOT further indicates UV emission lagging the X-rays by $5.9^{+4.1}_{-5.7}$ hours, consistent with disk reprocessing of coronal X-ray fluctuations, and corresponds to a light travel distance of up to $10^{3}\,r_{\rm g}$. Overall, our analysis maps the extent of the dynamically evolving absorber, the iron line emitter, and the accretion disk in this highly accreting NLSy1 system.
CommentsManuscript accepted for publication in The Astrophysical Journal. (20 pages, 9 figures, 2 tables)
