AI 中文总结
本研究利用VLT/MUSE及VLA数据，研究18个高光度2型类星体的电离外流，发现电子密度与外流速度正相关，强调准确电子密度测定对提升外流参数精度的重要性，为外流模拟提供参考。
AI 中文摘要
我们研究了一个包含18个光度（log L$_{\rm bol}$≥45 erg/s）的遮挡型类星体样本中的电离气体性质，这些样本红移范围为0.085<z<0.2，作为多波段类星体反馈巡天（QFeedS）的一部分，利用甚大望远镜（VLT）的多单元光谱探测器（MUSE）进行观测，并结合了甚大天线阵（VLA）的低分辨率和高分辨率数据。我们将外流相关量与文献报道的值进行比较，并研究外流与电离气体其他性质（如电子密度）之间可能存在的相关性。我们采用非参数方法表征由[O III]5007发射线示踪的电离气体运动学，并利用未分辨核光谱测量得到的$W_{80}$作为阈值，识别以外流为主的空间分辨单元（spaxels）。对射电图和$W_{80}$图的定性比较表明，总体而言，射电峰值与$W_{80}$峰值重合。我们将[O III]5007作为电离气体质量的示踪剂，通过两种不同方式获得外流相关性质：全局方式（采用流量加权速度和半径）和峰值方式（依赖径向剖面）。我们利用巴尔末减缩对[O III]5007流量进行消光校正。我们利用MUSE的灵敏度，仅在积分半径r=1.5''的光谱中可观测到的[Ar IV]4711、4740双线，测量每个星系的电子密度，得到$500<n_{e}{\rm[ cm^{-3}]}<27700$，进而得到外流率$0.03<\bar{M}_{\rm out}/{\rm (M_{\rm \bigodot} yr^{-1})}<4.17$，动能功率$39<\bar{E}_{\rm kin}/{\rm [erg/s]}<42$。我们的结果强调了准确确定电子密度的重要性，其导致外流率和动能功率出现约1个数量级的差异。我们观测到电子密度$n_e$与外流速度$V_{\rm out}$之间存在正相关，这被解释为高速下气体的压缩效应。这种相关性应在其他光度和红移范围内进一步研究，但可为未来的外流模拟研究提供参考。
英文摘要
We study ionised gas properties in a sample of 18 luminous (log L$_{\rm bol}\geq45$ erg/s) obscured QSOs at 0.085<z<0.2 observed with VLT/MUSE as part of the multi-wavelength Quasar Feedback Survey (QFeedS) and with VLA at low- and high-resolution data. We compare the outflow-related quantities with values reported in the literature and investigate possible correlations between the outflows and other properties of the ionised gas such as the electron density. We adopt a non-parametric approach to characterise the ionised gas kinematics, traced by the [O III]5007 emission line, and use $W_{80}$ measured from the unresolved nuclear spectra as a threshold to identify outflow-dominated spaxels. A qualitative comparison between the radio and the $W_{80}$ maps shows that, in general, the peak of the radio coincides with the peak of the $W_{80}$. The [O III]5007 is used as a proxy for the ionised gas mass, and the outflow-related properties are obtained in two different ways: the global, which uses flux-weighted velocities and radii; and the peak, relying on radial profiles. We correct the [O III]5007 flux for extinction using the Balmer decrement. We take advantage of the MUSE sensitivity and use the [Ar IV]4711,4740 doublet, only observable in the integrated r=1.5'' spectra, to measure the electron density in each galaxy. We obtain $500<n_{e}{\rm[ cm^{-3}]}<27700$, leading to 0.03$<\dot{M}_{\rm out}/{\rm (M_{\odot} yr^{-1})}<$4.17 and $39<\dot{E}_{\rm kin}/{\rm [erg/s]}<42$. Our results emphasise the importance of accurate n$_e$ determination, leading to a difference of ~1 dex in the outflow rates and kinetic powers. We observe a positive correlation between $n_e$ and $V_{\rm out}$, interpreted as compression of the gas at higher velocities. This correlation should be further investigated at other luminosity and redshift ranges, but it can inform future outflow simulation studies.
Comments23 pages, 23 figures (16 on the appendix), submitted to A&A
