论文标题
Seyfert Galaxy NGC 7130的复杂多组分流出
The complex multi-component outflow of the Seyfert galaxy NGC 7130
论文作者
论文摘要
AGN是理解银河进化的关键要素。 AGN驱动的流出是反馈的表现之一。 VLT的Muse的AO模式允许研究光学中附近AGN的最内向的数十个parsecs。我们对NGC 7130中央区域的离子气体进行了详细分析，NGC 7130，一个原型的复合材料Seyfert和核Starburst Galaxy。我们实现了0.17 $^{\ prime \ prime} $（50 pc）的角度分辨率。我们对主要ISM线进行了多组分分析，并确定了九个运动学组件，其中六个与流出相对应。流出是双形的，并且相对于光盘，速度为$ 100 \，{\ rm km \，s^{ - 1}} $。我们将流出的接近一侧分解为一个宽阔的狭窄组件，其典型速度分散剂在$ \ sim200 \，{\ rm km \，s^{ - 1}} $中，分别为$ \ sim200 \。蓝光狭窄的组件具有子结构，特别是与无线电射流对齐的准直羽流，表明它可能是喷射动力的。红移叶由两个狭窄的成分和一个宽的成分组成。在主流轴之外可以看到一个额外的红移组件。线比诊断表明，主轴中的流出气体为AGN供电，而离轴组件具有衬里特性。离子气体质量流出率为$ \ dot {m} = 1.2 \ pm0.7 \，m _ {\ odot} \，{\ rm yr yr^{ - 1}} $，动力是$ \ dot {e} kin} =（2.7 \ pm2.0）\ times10^{41} \，{\ rm erg \，s^{ - 1}} $，对应于$ f _ {\ rm kin} = 0.12 \ pm0.09 \ pm0.09 \％$ $ f _ {\ rm kin} \ pm0.09 \％$。高角度分辨率积分光谱和仔细的多组分分解的结合使NGC 7130中流出的详细介绍，这表明AGN运动学比传统上从不太复杂的数据和分析中得出的更为复杂。 （简略）
AGN are a key ingredient for understanding galactic evolution. AGN-driven outflows are one of the manifestations of feedback. The AO mode for MUSE at the VLT permits to study the innermost tens of parsecs of nearby AGN in the optical. We present a detailed analysis of the ionised gas in the central regions of NGC 7130, an archetypical composite Seyfert and nuclear starburst galaxy. We achieve an angular resolution of 0.17$^{\prime\prime}$ (50 pc). We performed a multi-component analysis of the main ISM lines and identified nine kinematic components, six of which correspond to the outflow. The outflow is biconic and has velocities of a few $100\,{\rm km\,s^{-1}}$ with respect to the disc. We decompose the approaching side of the outflow into a broad and a narrow component with typical velocity dispersions below and above $\sim200\,{\rm km\,s^{-1}}$, respectively. The blueshifted narrow component has substructure, in particular a collimated plume aligned with the radio jet, indicating that it may be jet-powered. The redshifted lobe is composed of two Narrow Components and a Broad Component. An additional redshifted component is seen outside the main outflow axis. Line ratio diagnostics indicate that the outflow gas in the main axis is AGN-powered whereas the off-axis component has LINER properties. The ionised gas mass outflow rate is $\dot{M}=1.2\pm0.7\,M_{\odot}\,{\rm yr^{-1}}$ and the kinetic power is $\dot{E}_{\rm kin}=(2.7\pm2.0)\times10^{41}\,{\rm erg\,s^{-1}}$, which corresponds to $F_{\rm kin}=0.12\pm0.09\%$ of the bolometric AGN power. The combination of high angular resolution integral field spectroscopy and a careful multi-component decomposition allows a uniquely detailed view of the outflow in NGC 7130, illustrating that AGN kinematics are more complex than traditionally derived from less sophisticated data and analyses. (abridged)
