论文标题
搜索五个Seyfert星系的核区域中/流出的分子气
Searching for molecular gas in/outflows in the nuclear regions of five Seyfert galaxies
论文作者
论文摘要
据信，以AGN驱动的流出主要通过负反馈来调节星系的增长，在调节星系的增长方面起着重要作用。但是，它们对宿主的影响远非清晰，尤其是对于低和中等的亮度Seyferts。为了研究这个问题，我们使用了CO（2-1）过渡所追踪的冷分子气体观测，使用附近的五个NOEMA干涉仪（19至58 MPC之间的距离）Seyfert星系。分辨率大约0.3-0.8 ARCSEC（约30-100 pc）和NOEMA的视野使我们能够研究核区域（约100 PC）中的CO（2-1）形态和运动学，并最高到径向距离。 900 PC。我们已经在所有五个星系中都检测到具有散光或环形环（如形态）的CO（2-1）。我们在核（大约100 pc）上得出了冷分子气体，并在$ 10^6 $到$ 10^7 $ m $ _ {\ odot} $中，从$ 10^6 $到$ 10^7 $到$ 10^7 $到$ 10^8 $ M _ $ M _ {\ odot} $。在我们所有的星系中，这种气体的大部分都在星系平面旋转。但是，也存在非圆周运动。在NGC 4253，NGC 4388和NGC 7465中，我们可以将流动作归因于大型棒的存在。在MRK 1066和NGC 4388中，由于AGN风与星系磁盘中的分子气体相互作用，核区域的非圆形运动被解释为流出的材料。我们得出的结论是，为了对冷分子气体的运动学做出明确而精确的解释，我们需要详细了解宿主星系（即，棒，相互作用等）以及电离气体运动学和电离锥体的电离。
AGN-driven outflows are believed to play an important role in regulating the growth of galaxies mostly via negative feedback. However, their effects on their hosts are far from clear, especially for low and moderate luminosity Seyferts. To investigate this issue, we have obtained cold molecular gas observations, traced by the CO(2-1) transition, using the NOEMA interferometer of five nearby (distances between 19 and 58 Mpc) Seyfert galaxies. The resolution of approx. 0.3-0.8 arcsec (approx. 30-100 pc) and field of view of NOEMA allowed us to study the CO(2-1) morphology and kinematics in the nuclear regions (approx. 100 pc) and up to radial distances of approx. 900 pc. We have detected CO(2-1) emission in all five galaxies with disky or circumnuclear ring like morphologies. We derived cold molecular gas masses on nuclear (approx. 100 pc) and circumnuclear (approx. 650 pc) scales in the range from $10^6$ to $10^7$M$_{\odot}$ and from $10^7$ to $10^8$ $M_{\odot}$, respectively. In all of our galaxies the bulk of this gas is rotating in the plane of the galaxy. However, non-circular motions are also present. In NGC 4253, NGC 4388 and NGC 7465, we can ascribe the streaming motions to the presence of a large-scale bar. In Mrk 1066 and NGC 4388, the non-circular motions in the nuclear regions are explained as outflowing material due to the interaction of the AGN wind with molecular gas in the galaxy disk. We conclude that for an unambiguous and precise interpretation of the kinematics of the cold molecular gas we need a detailed knowledge of the host galaxy (i.e., presence of bars, interactions, etc) as well as of the ionized gas kinematics and the ionization cone geometry.
