We present a HST/STIS spectroscopic and optical/radio imaging study of the Seyfert NGC 2110 aiming to measure the dynamics and understand the nature of the nuclear outflow in the galaxy. Previous HST studies have revealed the presence of a linear structure in the Narrow-Line Region (NLR) aligned with the radio jet. We show that this structure is strongly accelerated, probably by the jet, but is unlikely to be entrained in the jet flow. The ionisation properties of this structure are consistent with photoionisation of dusty, dense gas by the active nucleus. We present a plausible geometrical model for the NLR, bringing together various components of the nuclear environment of the galaxy. We highlight the importance of the circum-nuclear disc in determining the appearance of the emission line gas and the morphology of the jet. From the dynamics of the emission line gas, we place constraints on the accelerating mechanism of the outflow and discuss the relative importance of radio source synchrotron pressure, radio jet ram pressure and nuclear radiation pressure in accelerating the gas. While all three mechanisms can account for the energetics of the emission line gas, gravitational arguments support radio jet ram pressure as the most likely source of the outflow.
A deep, multi-epoch Chandra HETG study of the ionized outflow from NGC 4051
主动吸积的超大质量黑洞显著影响其宿主星系的演化，通过以广角流出排出大部分气体来截断进一步的恒星形成。X射线波段是理解这些黑洞风如何影响其环境的关键，因为流出物具有高温（$\sim$ 10 $^{5-8}$ K）。我们已经开发了一个贝叶斯框架，用于表征活动星系核（AGN）的外流，具有更好的探索参数空间和进行鲁棒模型选择的能力。我们将这个框架应用到一个新的700 ks和档案315 ks钱德拉高能透射光栅观测的塞弗特星系NGC 4051。我们已经检测到NGC 4051的六个固有吸收体。这些风分量的速度跨度从400 km s $^{-1}$到30，000 km s $^{-1}$。我们已经确定，统计上最重要的风分量是纯粹的碰撞电离，这是第一次检测到这样的吸收体。这种风具有$T\approx10^7$ K和$v\approx880$ km s $^{-1}$，并且在两个时期之间保持非常稳定。其他慢分量也随时间保持稳定。快速外流成分在2008年至2016年之间改变了它们的性质，这表明要么是物理变化，要么是云在视线范围内移动。对于其中一个快速分量，我们获得了迄今为止最严格的风密度测量值之一，log $n/$ [cm $^{-3}$ ]=13.0 $^{+0.01}_{-0.02}$，并确定它位于$\sim$ 240引力半径处。估计总流出功率超过5%的热光度（尽管有很大的不确定性），使其在星系-黑…
Outflowing shocked gas dominates the NIR H$_2$ emission from the dual AGN NGC6240
Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）；European Southern Observatory (ESO)（欧洲南方天文台）；National and Kapodistrian University of Athens（雅典国立卡波蒂斯坦大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Università degli Studi di Bologna（博洛尼亚大学）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学天文台）；ASTRON, The Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Kapteyn Astronomical Institute（卡普坦天文研究所）；University of South Carolina（南卡罗来纳大学）
