AGN STORM 2. VII. Mrk 817 吸积盘的频率分辨图：X 射线混响与 UVOIR 盘再处理时间延迟的同步测量
AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-ray Reverberation and UVOIR Disk Reprocessing Time Lags
AI总结：
该研究基于 AGN STORM 2 对 Mrk 817 的多波段同步监测，首次联合 X 射线混响与 UVOIR 再处理延迟，揭示黑洞全吸积盘结构及电离外流和 BLR 对延迟的影响。
摘要：
X 射线混响映射是探测最内侧吸积盘的强大技术，而紫外、光学和红外（UVOIR）连续谱混响映射则揭示吸积盘其余部分及宽线区（BLR）的再处理。作为 AGN STORM 2 活动的一部分，我们利用 Swift 和地面望远镜 14 个月的高频次监测，以及一次 XMM-Newton 观测，给出了 Mrk 817 的时间延迟随时间频率变化的函数。XMM-Newton 延迟首次在该源中探测到软延迟，与来自最内侧吸积流的混响相符。这些结果标志着首次同步测量 X 射线混响与 UVOIR 盘再处理延迟——实际上使我们能够绘制黑洞周围整个吸积盘的分布图。与以往的连续谱混响映射活动类似，在低时间频率处产生的 UVOIR 时间延迟比标准盘再处理预期值长 2–3 倍。当分离短时间尺度变化（即短于 Hβ 延迟的时间尺度）时，这些延迟与预期的盘混响延迟一致。对延迟进行建模需要额外的再处理成分，其约束半径与同期 Hβ 延迟测量推断的 BLR 尺度相符。当我们划分活动光变曲线时，UVOIR 延迟表现出显著变化：在电离外流造成的遮蔽最强时测得的延迟更长。我们认为，当遮蔽体最强时，BLR 的再处理最显著地拉长了延迟；随着风减弱，延迟则由更短的吸积盘延迟主导。
英文摘要：
X-ray reverberation mapping is a powerful technique for probing the innermost accretion disk, whereas continuum reverberation mapping in the UV, optical, and infrared (UVOIR) reveals reprocessing by the rest of the accretion disk and broad-line region (BLR). We present the time lags of Mrk 817 as a function of temporal frequency measured from 14 months of high-cadence monitoring from Swift and ground-based telescopes, in addition to an XMM-Newton observation, as part of the AGN STORM 2 campaign. The XMM-Newton lags reveal the first detection of a soft lag in this source, consistent with reverberation from the innermost accretion flow. These results mark the first simultaneous measurement of X-ray reverberation and UVOIR disk reprocessing lags$\unicode{x2013}$effectively allowing us to map the entire accretion disk surrounding the black hole. Similar to previous continuum reverberation mapping campaigns, the UVOIR time lags arising at low temporal frequencies are longer than those expected from standard disk reprocessing by a factor of 2-3. The lags agree with the anticipated disk reverberation lags when isolating short-timescale variability, namely timescales shorter than the H$β$ lag. Modeling the lags requires additional reprocessing constrained at a radius consistent with the BLR size scale inferred from contemporaneous H$β$-lag measurements. When we divide the campaign light curves, the UVOIR lags show substantial variations, with longer lags measured when obscuration from an ionized outflow is greatest. We suggest that, when the obscurer is strongest, reprocessing by the BLR elongates the lags most significantly. As the wind weakens, the lags are dominated by shorter accretion disk lags.
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