论文标题
MCG-03-58-007的分层磁盘风
The stratified disk wind of MCG-03-58-007
论文作者
论文摘要
过去的Suzaku，XMM和Nustar的观测值（Z = 0.0323）Bright Seyfert 2 Galaxy MCG-03-58-007显示出存在两个深层和蓝色的Fe K-Shell吸收线轮廓。这些可以用高度电离的高柱密度积聚磁盘的两个阶段的存在，并用$ v_ {out1} \ sim -0.1c $和$ v_ {out2} \ sim -0.2c $流出。在这里，我们介绍了MCG-03-58-007的两个新观察：2016年与Chandra一起进行了一次，并在2018年与Swift一起进行。两者都以更明亮的状态捕获了MCG-03-58-007（$ f _ {\ mathrm {2-10 \，kev}}} \ sim 4 \ sim 4 \ times 10^{ - 12} $ erg cm $^{ - 2} $ s $ s $ s $ s $ s $ s $^{ - 1} $）令人震惊的是fastk fastk fastk fastk wistk fastk wine of fastek wind of fastek wind of fastek wine。然后分析了涵盖2010年至2018年期间的MCG-03-58-007的多个观测值。这些数据表明，较低的速度组件以$ v_ {out1} \ sim -0.072 \ pm 0.002c $流出，但在所有观察值中都是持久的，并且在所有观察值中都检测到，尽管它在列密度范围内变量$ n_ \ rm {在2016年的快速观察中，我们再次检测到第二个更快的组件，其中$ v_ {out2} \ sim -0.2c $流出，列密度（$ n_ \ rm {h} = 7.0^{+5.6} _ {+5.6} _ { - 4.1} \ 4.1} \ times 10^{23} $ cm $ cm $ cm $ cm^{-2}但是，在两年前的钱德拉观察期间，该区域不存在（$ n_ \ rm {h} <1.5 \ times 10^{23} $ cm $^{ - 2} $），这表明此更快的区域是间歇性的。总体而言，多上点观察结果表明，MCG-03-58-007中的磁盘风不仅功能强大，而且可变也很大，因此将MCG-03-58-007置于独特的磁盘中，例如在著名的QSO PDS456中看到的磁盘风。这项调查的主要结果之一是考虑到这些风可能是极大的，有时会出现并且有时消失。因此，为了得出关于其能量学的坚实和坚定的结论，必须进行多个观察。
Past Suzaku, XMM and NuSTAR observations of the nearby (z=0.0323) bright Seyfert 2 galaxy MCG-03-58-007 revealed the presence of two deep and blue-shifted Fe K-shell absorption line profiles. These could be explained with the presence of two phases of a highly ionized, high column density accretion disk wind outflowing with $v_{out1}\sim -0.1c$ and $v_{out2}\sim -0.2c$. Here we present two new observations of MCG-03-58-007: one was carried out in 2016 with Chandra and one in 2018 with Swift. Both caught MCG-03-58-007 in a brighter state ($F_{\mathrm{2-10\,keV}}\sim 4\times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$) confirming the presence of the fast disk wind. The multi-epoch observations of MCG-03-58-007 covering the period from 2010 to 2018 were then analysed. These data show that the lower velocity component outflowing with $v_{out1}\sim -0.072\pm 0.002c$ is persistent and detected in all the observations, although it is variable in column density in the range $N_\rm{H}\sim 3-8 \times 10^{23}$cm$^{-2}$. In the 2016 Swift observation we detected again the second faster component outflowing with $v_{out2}\sim -0.2c$, with a column density ($N_\rm{H}=7.0^{+5.6}_{-4.1}\times 10^{23}$cm$^{-2}$), similar to that seen during the Suzaku observation. However during the Chandra observation two years earlier, this zone was not present ($N_\rm{H}<1.5\times 10^{23}$cm$^{-2}$), suggesting that this faster zone is intermittent. Overall the multi-epochs observations show that the disk wind in MCG-03-58-007 is not only powerful, but also extremely variable, hence placing MCG-03-58-007 among unique disk winds such as the one seen in the famous QSO PDS456. One of the main results of this investigation is the consideration that these winds could be extremely variable, sometime appearing and sometime disappearing; thus to reach solid and firm conclusions about their energetics multiple observations are mandatory.
