论文标题
活性核与宿主星系星际培养基的相互作用
The interaction of the active nucleus with the host galaxy interstellar medium
论文作者
论文摘要
附近AGN的成像X射线光谱（主要是Chandra）表明，延长的软（<2.5 keV）发射线主导的X射线双色质结构（Kiloparsec量表）在高度吸收的康普顿（Compton）厚度（CT）AGN中很普遍。 X射线发射很复杂，需要光电离电气和电离气体。它起源于高电离区域，被低电离狭窄线发射区（衬里）的茧所包围。 Bicone 3-6 KEV连续体和6.4 Kev Fe Kalpha排放已被检测到，与标准AGN模型的预期相反，该预期将使这种硬发射限制在PC大小的核吸收圆环中。在跨杆方向上的扩展发射也需要对AGN标准模型进行修改。似乎需要一个多孔的圆环，其中很大一部分逃脱了AGN连续体，并且与ISM的喷气相互作用似乎需要向核区域产生吹回去。在这里，我们讨论了这些结果及其对AGN模型的影响以及我们对AGN反馈的理解。在10s parsec上发现热量和高度光电离的气体对几千座尺度的发现表明，所有三种反馈机制都在起作用：辐射会影响宿主的内部分子云，以约1 kpc的量表；相对论喷气机与主机ISM的震动来自中央AGN的几个KPC； ISM通过从PC到多个KPC的尺度上的风将ISM进行光电离。这些结果表明，需要X射线与无线电连续体，MM和Sub-MM分子线发射以及光学/接近IR发射线一起开发AGN/宿主相互作用的完整图片。
Imaging X-ray spectroscopy of nearby AGNs, mostly with Chandra, has shown that extended soft (<2.5 keV) emission-line dominated X-ray biconical structures, of kiloparsec scale, are widespread in highly absorbed Compton Thick (CT) AGNs. The X-ray emission is complex, requiring both photoionized and shock-ionized gas. It originates from high ionization regions and is surrounded by cocoons of low ionization narrow line emission regions (LINERS). Bicone 3-6 keV continuum and 6.4 keV Fe Kalpha emission has been detected, contrary to the standard AGN model expectation that would confine this hard emission to the pc-size nuclear absorbing torus. Extended emission in the cross-cone direction, also requires modifications to the AGN standard model. A porous torus, with a significant fraction of escaping AGN continuum, and/or jet interaction with ISM creating a blow-back towards the nuclear region seem to be required. Here we discuss these results and their implications for both the AGN model and our understanding of AGN feedback. The finding of hot and highly photoionized gas on 10s parsecs to several kiloparsec scales demonstrates that all three feedback mechanisms are at work: radiation affects the inner molecular clouds of the host on a ~1 kpc scale; shocks of relativistic jets with the host ISM a few kpc from the central AGN; and photoionization of the ISM via winds on scales from pc to multiple kpc. These results demonstrate that X-rays are needed to develop a complete picture of AGN/host interaction along with radio continuum, mm and sub-mm molecular line emission, and optical/near-IR emission lines.
