来自AGN的外流：塞弗特星系窄线区和日冕线区的运动学
Outflows from AGN: Kinematics of the Narrow-Line and Coronal-Line Regions in Seyfert Galaxies
摘要：
作为活动星系核物理性质广泛研究的一部分，我们报道了7个Seyfert星系窄线区和冕线区的高空间分辨率近红外积分场光谱。这些测量首次阐明了活动星系核尺度<300 pc的Brγ复合线和高电离线[Sivi]、[Alix]和[Caviii]的二维空间分布和运动学。观测结果揭示了NLR和NLR中旋转和外流的运动学特征。空间分辨的运动学可以建模为流出双锥和与分子气体重合的旋转盘的组合。在这两种成分中都可以看到高激发发射，这表明它是从一个cluterectorus中泄漏出来的。虽然NGC 1068（塞弗特2）几乎是从侧面观察的，但中间型塞弗特是从中间角度观察的，与统一的方案一致。在r<30 pc时，外流速度与分子气体质量之间的相关性表明，活动星系核周围气体的聚集增加了外流的准直性和速度。外流速率比吸积速率大2-3个数量级，这意味着外流是由周围的星际介质（ISM）的质量加载。在观测到的活动星系核的一半中，外流的动力学功率是两级反馈模型与ISM热耦合并匹配M-σ* 关系所需功率的量级。在这些物体中，无线电喷流显然与ISM相互作用，表明喷流功率和外流功率之间存在联系。
英文摘要：
As part of an extensive study of the physical properties of active galactic nuclei (AGN) we report high spatial resolution near-IR integral-field spectroscopy of the narrow-line region (NLR) and coronal-line region (CLR) of seven Seyfert galaxies. These measurements elucidate for the first time the two-dimensional spatial distribution and kinematics of the recombination line Brγ and high-ionization lines [Sivi], [Alix] and [Caviii] on scales <300 pc from the AGN. The observations reveal kinematic signatures of rotation and outflow in the NLR and CLR. The spatially resolved kinematics can be modeled as a combination of an outflow bicone and a rotating disk coincident with the molecular gas. High-excitation emission is seen in both components, suggesting it is leaking out of a clumpy torus. While NGC 1068 (Seyfert 2) is viewed nearly edge-on, intermediate-type Seyferts are viewed at intermediate angles, consistent with unified schemes. A correlation between the outflow velocity and the molecular gas mass in r<30 pc indicates that the accumulation of gas around the AGN increases the collimation and velocity of the outflow. The outflow rate is 2-3 orders of magnitude greater than the accretion rate, implying that the outflow is mass-loaded by the surrounding interstellar medium (ISM). In half of the observed AGN the kinetic power of the outflow is of the order of the power required by two-stage feedback models to be thermally coupled to the ISM and match the M-σ* relation. In these objects the radio jet is clearly interacting with the ISM, indicative of a link between jet power and outflow power.
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