论文标题
X射线风在遥远的类星体中：第一个高红移风周期
X-raying winds in distant quasars: the first high-redshift wind duty cycle
论文作者
论文摘要
来自活性银河核（AGN）的风向反馈的理论模型通常将超快速流出（UFOS）视为产生星系大小流出的主要原因，这可能是建立所谓的AGN-Galaxy共同进化的主要参与者。不明飞行物在本地AGN中的特征很好，但是在SF和AGN活动达到顶峰的宇宙时间（$ z \ simeq1-3 $）的宇宙时期，不明飞行物的特征少得多。因此，必须在高$ z $来源中搜索不明飞行物的证据以测试风向驱动的AGN反馈模型。在这里，我们提出了一项研究Q2237+030，Einstein Cross，这是一项四倍成像的无线电广播镜头，位于$ z = 1.695 $。我们对所有可用的Chandra和XMM-Newton数据（截至2019年9月）进行了系统和全面的时间和空间解决的X射线光谱分析。我们发现了光谱变异性的明确证据，这可能是由于吸收柱密度（或覆盖分数）固有的可变性所致。我们在此类星体中第一次检测到$ v _ {\ rm out} \ simeq0.1c $的快速X射线，将足够强大（$ \ dot {e} _ {\ dot {e} _ {\ rm kin} \ simeq0.1 l _ {我们还报告了风的可能存在更快的组件（$ v _ {\ rm out} \ sim0.5c $）。鉴于分析的X射线数据跨越了较大的样本和长时间的间隔，我们能够在高$ z $ quasar中首次大致估算，而风行周期为$ \ of $ \ of your of0.46 \，（0.31）$，$ 90 \％\％\，（95 \％\％）$ funstrus fusits $。最后，我们还证实了具有可变能量的Fe K $α$发射线的存在，我们根据微透镜效应进行了讨论，并考虑了我们在源上的发现。
Theoretical models of wind-driven feedback from Active Galactic Nuclei (AGN) often identify Ultra-fast outflows (UFOs) as being the main cause for generating galaxy-size outflows, possibly the main actors in establishing the so-called AGN-galaxy co-evolution. UFOs are well characterized in local AGN but much less is known in quasars at the cosmic time when SF and AGN activity peaked ($z\simeq1-3$). It is therefore mandatory to search for evidences of UFOs in high-$z$ sources to test the wind-driven AGN feedback models. Here we present a study of Q2237+030, the Einstein Cross, a quadruply-imaged radio-quiet lensed quasar located at $z=1.695$. We performed a systematic and comprehensive temporally and spatially resolved X-ray spectral analysis of all the available Chandra and XMM-Newton data (as of September 2019). We find clear evidence for spectral variability, possibly due to absorption column density (or covering fraction) variability intrinsic to the source. We detect, for the first time in this quasar, a fast X-ray wind outflowing at $v_{\rm out}\simeq0.1c$ that would be powerful enough ($\dot{E}_{\rm kin}\simeq0.1 L_{\rm bol}$) to significantly affect the host galaxy evolution. We report also on the possible presence of an even faster component of the wind ($v_{\rm out}\sim0.5c$). Given the large sample and long time interval spanned by the analyzed X-ray data, we are able to roughly estimate, for the first time in a high-$z$ quasar, the wind duty cycle as $\approx0.46\,(0.31)$ at $90\%\,(95\%)$ confidence level. Finally, we also confirm the presence of a Fe K$α$ emission line with variable energy, which we discuss in the light of microlensing effects as well as considering our findings on the source.
