Variability of the X-ray obscuring wind in Mrk 335 with XMM-Newton/RGS
University of Chicago（芝加哥大学）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Saint Mary’s University（圣玛丽大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；The Ohio State University（俄亥俄州立大学）；Technion（以色列理工学院）
Daniele Rogantini, Erin Kara, Luigi Gallo, S Komossa, Peter Kosec, Christos Panagiotou, Dan Wilkins, Ehud Behar, Joheen Chakraborty, Dirk Grupe, Missagh Mehdipo… 展开作者
Daniele Rogantini, Erin Kara, Luigi Gallo, S Komossa, Peter Kosec, Christos Panagiotou, Dan Wilkins, Ehud Behar, Joheen Chakraborty, Dirk Grupe, Missagh Mehdipour, Ciro Pinto, Irina Zhuravleva
Transient X-ray obscuration in Seyfert 1 galaxies likely arises from clumpy accretion-disk winds near the broad-line region (BLR), but the wind structure and short-timescale variability are difficult to measure because high-resolution spectra are often suppressed during deep low states. We analyse a coordinated XMM-Newton/NuSTAR campaign on Mrk 335 in June 2021, with long-term Swift monitoring, capturing the source in an intermediate-flux state with strong RGS absorption features. We model the broadband SED to determine the ionising continuum for self-consistent photoionisation modelling of the RGS spectra. The stacked RGS spectrum requires three photoionised absorbers with log xi ~ 3.69, 2.97, and 1.91, outflowing at |v_out| ~ 5800, 3200, and 2100 km/s, respectively. Their properties are consistent with the three-phase obscurer reported in 2009, indicating that a similar multi-phase obscuring wind can persist over decade timescales. Using five consecutive RGS observations, we track the wind evolution on day timescales and find strong variability in column density and ionisation in all phases, together with smaller but coherent velocity changes. During a flare, the low-ionisation phase shows a significant drop in opacity, while in the subsequent epoch all phases show increased outflow velocities, suggesting a possible connection between continuum variability and changes in the line-of-sight absorber. The high-ionisation phase responds most directly to changes in ionising luminosity, while the lowest-ionisation phase shows at most a delayed response. Order-of-magnitude constraints place the obscurer at BLR scales, ~10^3-10^5 Rg, with kinetic power potentially reaching the percent level of L_bol for plausible assumptions on geometry and clumpiness.
Variable oxygen emission from the accretion disk of Mrk 110
给出了2004-2020年期间对明亮窄线Seyfert 1（Mrk 110）的六次XMM-牛顿观测结果。从反射光栅光谱仪（RGS）的光栅光谱的分析揭示了一个广泛的组成部分，类氦氧（OVII）线，与半高宽（FWHM）的$15900\pm1800$ km s $^{-1}$测量的平均光谱。在所有六个观测中的宽OVII线可以用一个正面的吸积盘轮廓来模拟，从这些轮廓中可以推断出线发射的内半径位于距离黑洞大约20-100个引力半径之间。推导出的倾斜角，约10度，是一致的，在Mrk 110的光学宽线区的研究。该线也出现变量，并为第一次，一个显着的相关性之间的OVII通量和连续通量从RGS和EPIC-pn数据进行测量。因此，该线响应于连续谱，当连续谱通量最高时最亮，类似于所报道的光学HeII线的行为。线发射气体的密度估计为$n_{\rm e}\sim10^{14}$ cm $^{-3}$，与吸积盘的起源一致。
Dynamic Accretion Disk-Corona Connection and Broad Fe K$α$ Variability in Mrk 766 Revealed by Time-Resolved High Resolution X-Ray Spectroscopic Analysis
University of Maryland Baltimore County（马里兰大学巴尔的摩分校）；School of Astrophysics, Presidency University（总统大学天体物理学院）；Inter-University Centre for Astronomy and Astrophysics (IUCAA)（大学间天文与天体物理中心）
