论文标题
Wissh Quasars项目X.发现多组分和高度变化的UV Ultra-Fast流出Z = 3.6 Quasar
The WISSH quasars project X. Discovery of a multi-component and highly-variable UV ultra-fast outflow in a z=3.6 quasar
论文作者
论文摘要
我们报告在z = 3.6时观察到的多组分宽吸收系（BAL）系统的多组分宽吸收系（BAL）系统的变异性。提出了从SDS，VLT，LBT和Subaru望远镜以五个不同时期进行的观察结果，在观察到的框架中跨越了17年。我们检测到三个（a，b，c）CIV变量槽，表现出极端速度（$ \ sim $ 40,000-54,000 km s $^{ - 1} $），类似于X射线光谱中通常观察到的Ultra-fast Offlows（UFOS）。 The A component of the BAL UFO ($\rm v_{ufo}$ $\sim$0.17 c) shows strength variations, while B ($\rm v_{ufo}$ $\sim$0.15 c) and C ($\rm v_{ufo}$ $\sim$0.13 c) components show changes both in shape and strength, appearing and disappearing at different时代。此外，在2021年6月的最后一次观察中，整个BAL系统消失了。在CIV，SIIV，OVI和NV吸收光谱区域中的前两个时期（1.30年休息框架）期间观察到的可变性趋势是B和C槽相同的，而BAL的A组分则独立不同。这表明B和C分量吸收气体的电离状态发生了变化，并且A组分的切向运动是这种时间行为的原因。因此，可以为$ rm_ {out}^{a} $ 5 \ le $ 58 pc的A组件的气体的距离提供一个上限s $ \ rm^{ - 1} $。我们还获得了$ r \ rm_ {out}^{b，c} $ $ \ le $ 2.7 kpc for B和c组件，这意味着上限的上限估计为$ \ dot {e} \ rm_ {k，k，ufo} $ \ dot {e} \ rm_ {k，ufo} $ $ \ le $ \ le $ 1.4 $ \ times $ 10 $^{46} $ erg s $ \ rm \ rm^{ - 1} $。必须使用高分辨率仪器进行未来的光谱监测，以准确限制J1538+0855紫外线光谱中发现的BAL UFO的物理特性。
We report on the variability of a multi-component broad absorption line (BAL) system observed in the hyper-luminous quasar J1538+0855 at z=3.6. Observations from SDSS, VLT, LBT and Subaru telescopes taken at five different epochs, spanning 17 yr in the observed frame, are presented. We detect three (A, B, C) CIV variable troughs exhibiting extreme velocities ($\sim$40,000-54,000 km s$^{-1}$) similar to the ultra-fast outflows (UFOs) typically observed in the X-ray spectra. The A component of the BAL UFO ($\rm v_{ufo}$ $\sim$0.17 c) shows strength variations, while B ($\rm v_{ufo}$ $\sim$0.15 c) and C ($\rm v_{ufo}$ $\sim$0.13 c) components show changes both in shape and strength, appearing and disappearing at different epochs. In addition, during the last observation on June 2021 the entire BAL system disappears. The variability trends observed during the first two epochs (1.30 yr rest-frame) in the CIV, SiIV, OVI and NV absorption spectral regions are the same for B and C troughs, while the A component of the BAL varies independently. This suggests a change in the ionization state of the absorbing gas for B and C components and tangential motion for the A component, as causes of this temporal behavior. Accordingly, it is possible to provide an upper limit for distance of the gas responsible for the A component of $R\rm_{out}^{A}$$\le$58 pc, and in turn, a kinetic power of $\dot{E}\rm_{K,ufo}$ $\le$5.2 $\times$ 10$^{44}$ erg s$\rm^{-1}$. We also obtain $R\rm_{out}^{B,C}$ $\le$2.7 kpc for B and C components, which implies an upper limit estimation of $\dot{E}\rm_{K,ufo}$ $\le$2.1$\times$10$^{46}$ erg s$\rm^{-1}$ and $\dot{E}\rm_{K,ufo}$ $\le$1.4$\times$10$^{46}$ erg s$\rm^{-1}$, respectively. Future spectral monitoring with high-resolution instruments is mandatory to accurately constrain physical properties of the BAL UFO discovered in the UV spectrum of J1538+0855.
