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arXiv 2303.07098astro-ph.GA
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UGC 8782射电大声AGN中外流的空间分辨观测

Spatially resolved observations of outflows in the radio loud AGN of UGC 8782

Rogemar A. Riffel, Rogério Riffel, Marina Bianchin, Thaisa Storchi-Bergmann, Gabriel Luan Souza de Oliveira, Nadia L. Zakamska

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Accepted for publication by MNRAS
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摘要：

利用光学积分场谱（IFU）研究了射电大活动星系核（AGN）的宿主星系UGC 8782（3C 293）的内部3.4 $\times$ 4.9 kpc $^2$区域的气体发射结构和运动学。观测是用双子座北望远镜上的GMOS-IFU进行的，结果在星系距离上的空间分辨率为$\sim725$ pc。虽然恒星呈现有序的旋转方向的大规模磁盘，气体显示出扰动的运动学。发射线的配置文件提出了两个运动学的组成部分：一个狭窄的（$σ\lesssim200$公里的$^{-1}$）组件与气体中的磁盘的星系和广泛的（$σ\gtrsim200$公里的$^{-1}$）组件产生的气体流出。发射线比图表明，圆盘中的气体被活动星系核辐射场激发，而外流的发射包括由于射电喷流与环境气体相互作用而产生的冲击激发的额外贡献。从纯旋转的偏差，高达30公里秒$^{-1}$，观察在光盘组件和可能产生的前合并事件。广泛的组件是蓝移的$\sim150-500$公里的$^{-1}$相对于星系的系统速度在所有位置。我们构造了电离气体流出的质量流出率和动能功率的径向分布，它们在离核的$\sim1$ kpc处有最大值，峰值为$\dot{M}_{\rm out,ΔR}=0.5\pm0.1$ M $_\odot$ yr $^{-1}$和$\dot{K}_{\rm out,ΔR} =$（6.8 $\pm$ 1.1）$\times$ 10 $^{41}$ erg s $^{-1}$。这些外流的动力学耦合效率在1 $-$ 3%的范围内，这表明它们可能足够强大，足以影响宿主星系中的恒星形成，正如理论模拟所预测的那样。

英文摘要：

We use optical Integral Field Spectroscopy (IFU) to study the gas emission structure and kinematics in the inner 3.4$\times$4.9 kpc$^2$ region of the galaxy UGC 8782 (3C 293), host of a radio loud Active Galactic Nucleus (AGN). The observations were performed with the GMOS-IFU on the Gemini North telescope, resulting in a spatial resolution of $\sim725$ pc at the distance of the galaxy. While the stars present ordered rotation following the orientation of the large scale disc, the gas shows a disturbed kinematics. The emission-line profiles present two kinematic components: a narrow ($σ\lesssim200$ km s$^{-1}$) component associated with the gas in the disc of the galaxy and a broad ($σ\gtrsim200$ km s$^{-1}$) component produced by gas outflows. Emission-line ratio diagrams indicate that the gas in the disc is excited by the AGN radiation field, while the emission of the outflow includes additional contribution of shock excitation due to the interaction of the radio jet with the environment gas. Deviations from pure rotation, of up to 30 km s$^{-1}$, are observed in the disc component and likely produced by a previous merger event. The broad component is blueshifted by $\sim150-500$ km s$^{-1}$ relative to the systemic velocity of the galaxy in all locations. We construct radial profiles of the mass outflow rate and kinetic power of the ionized gas outflows, which have the maximum values at $\sim1$ kpc from the nucleus with peak values of $\dot{M}_{\rm out,ΔR}=0.5\pm0.1$ M$_\odot$ yr$^{-1}$ and $\dot{K}_{\rm out,ΔR} =$(6.8$\pm$1.1)$\times$10$^{41}$ erg s$^{-1}$. The kinetic coupling efficiency of these outflows is in the range of 1$-$3 per cent, indicating that they could be powerful enough to affect the star formation in the host galaxy as predicted by theoretical simulations.

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