Ultrafast outflows in radio-loud active galactic nuclei
Ultrafast outflows in radio-loud active galactic nuclei
复制标题
DOI：
10.1093/mnras/stu1297
复制
发表时间：
2014-06
影响因子：
4.8
通讯作者：
F. Tombesi;F. Tazaki;R. Mushotzky;Y. Ueda;M. Cappi;J. Gofford;J. Reeves;M. G. Nasagsfc;D. Astr
中科院分区：
文献类型：
--
作者：
F. Tombesi;F. Tazaki;R. Mushotzky;Y. Ueda;M. Cappi;J. Gofford;J. Reeves;M. G. Nasagsfc;D. Astr
最近的 X 射线观测表明，在 6 个宽线射电星系的有限样本中，吸收风的速度高达约 0.1c 的轻度相对论值。它们被观察为蓝移的 Fe XXV-XXVI K 壳吸收线，类似于 Seyferts 和类星体中报道的超快外流 (UFO)。在这项工作中，我们将对此类 Fe K 吸收线的搜索扩展到使用 XMM-Newton 和 Suzaku 观察到的 26 个无线电响 AGN 的更大样本。样本取自 Swift BAT 58 个月目录，不包括耀变体。 X 射线明亮的 FR II 射电星系构成了大部分来源。将此分析结果与文献中的结果相结合，我们发现在 >27% 的来源中检测到了 UFO。然而，通过校正信噪比不足的频谱数量，我们可以估计 UFO 的发生率是无线电响亮 AGN 的样本，其范围可能在 f=(50+/-20)% 范围内。使用 XSTAR 对吸收线进行光电离建模，可以估计其主要参数的分布。观察到的流出速度广泛分布在 v_out 10^22 cm^-2 之间。总体而言，这些特征与很大一部分射电强活动星系核中复杂的吸积盘风的存在相一致，并且根据几个理论模型，证明相对论性喷流的存在并不排除风的存在。
Recent X-ray observations show absorbing winds with velocities up to mildly-relativistic values of the order of ~0.1c in a limited sample of 6 broad-line radio galaxies. They are observed as blue-shifted Fe XXV-XXVI K-shell absorption lines, similarly to the ultra-fast outflows (UFOs) reported in Seyferts and quasars. In this work we extend the search for such Fe K absorption lines to a larger sample of 26 radio-loud AGNs observed with XMM-Newton and Suzaku. The sample is drawn from the Swift BAT 58-month catalog and blazars are excluded. X-ray bright FR II radio galaxies constitute the majority of the sources. Combining the results of this analysis with those in the literature we find that UFOs are detected in >27% of the sources. However, correcting for the number of spectra with insufficient signal-to-noise, we can estimate that the incidence of UFOs is this sample of radio-loud AGNs is likely in the range f=(50+/-20)%. A photo-ionization modeling of the absorption lines with XSTAR allows to estimate the distribution of their main parameters. The observed outflow velocities are broadly distributed between v_out 10^22 cm^-2. Overall, these characteristics are consistent with the presence of complex accretion disk winds in a significant fraction of radio-loud AGNs and demonstrate that the presence of relativistic jets does not preclude the existence of winds, in accordance with several theoretical models.