论文标题
解决PDS 456中的软X射线超快速流出
Resolving the soft X-ray ultra fast outflow in PDS 456
论文作者
论文摘要
过去对附近发光的Quasar PDS 456（$ z = 0.184 $）的X射线观察显示，广角积聚磁盘风（Nardini等人，2015年），流出速度为$ \ sim-0.25c $，正如通过观察到其蓝色蓝光的铁K-shell吸收型线的观察所观察到的。在这里，我们提出了PDS 456的三个新的XMM-Newton观察结果；一个在2018年9月的一个，即类星体明亮且毫无特色，2019年9月相隔22天，当时是类星体五次昏昏欲睡的情况下发生的，而风中有强烈的蓝换线线。在2019年9月的第二次观察中，在高分辨率RGS Spectrum中解析了三个宽（$σ= 3000 $ km s $^{ - 1} $）的吸收线，它们用蓝色变为蓝色的oviii ly $α$，neix he $α$α$和nex ly $ ly $ ly $α$确定。发现此软X射线吸收器的流出速度为$ v/c = -0.258 \ pm0.003 $，完全与$ v/c = -0.261 \ pm0.007 $的铁K吸收器完全一致。软X射线组件的电离参数和列密度（$ \logξ= 3.4 $，$ n _ {\ rm h} = 2 \ 2 \ times10^{21} $ cm $^{ - 2} $）的流出较低降低了大约两个较大的阶，与Inrodiatization k的高离子k（$ \ log \ log \ ym）相比h} = 7 \ times10^{23} $ cm $^{ - 2} $）。在2019年观察结果之间的软X射线吸收器中看到了实质性可变性，从$ n _ {\ rm h} = 10^{23} $ cm $^{ - 2} $到$ n _ {\ rm h} = 10^{21} $ cm $ cm $^{ - 2} $ compocent at Irond st Ironports componcend stancecondion我们得出的结论是，柔软的X射线风可能源于视线穿过视线的不均匀风流，并且由于其较低的电离，它距离黑洞更远，而不是parsec尺度，而不是最内向的磁盘。
Past X-ray observations of the nearby luminous quasar PDS 456 (at $z=0.184$) have revealed a wide angle accretion disk wind (Nardini et al. 2015), with an outflow velocity of $\sim-0.25c$, as observed through observations of its blue-shifted iron K-shell absorption line profile. Here we present three new XMM-Newton observations of PDS 456; one in September 2018 where the quasar was bright and featureless, and two in September 2019, 22 days apart, occurring when the quasar was five times fainter and where strong blue-shifted lines from the wind were present. During the second September 2019 observation, three broad ($σ=3000$ km s$^{-1}$) absorption lines were resolved in the high resolution RGS spectrum, which are identified with blue-shifted OVIII Ly$α$, NeIX He$α$ and NeX Ly$α$. The outflow velocity of this soft X-ray absorber was found to be $v/c=-0.258\pm0.003$, fully consistent with iron K absorber with $v/c=-0.261\pm0.007$. The ionization parameter and column density of the soft X-ray component ($\logξ=3.4$, $N_{\rm H}=2\times10^{21}$ cm$^{-2}$) outflow was lower by about two orders of magnitude, when compared to the high ionization wind at iron K ($\logξ=5$, $N_{\rm H}=7\times10^{23}$ cm$^{-2}$). Substantial variability was seen in the soft X-ray absorber between the 2019 observations, declining from $N_{\rm H}=10^{23}$ cm$^{-2}$ to $N_{\rm H}=10^{21}$ cm$^{-2}$ over 20 days, while the iron K component was remarkably stable. We conclude that the soft X-ray wind may originate from an inhomogeneous wind streamline passing across the line of sight and which due to its lower ionization, is located further from the black hole, on parsec scales, than the innermost disk wind.
