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arXiv 1802.00486astro-ph.GA
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ALMA [ CI ]对塞弗特星系中心区域的观测NGC 613

ALMA [CI] observations toward the central region of a Seyfert galaxy NGC 613

Yusuke Miyamoto, Masumichi Seta, Naomasa Nakai, Yoshimasa Watanabe, Dragan Salak, Shun Ishii

备注：
6 pages, 4 figures, 1 supplement material, Accepted for publication in PASJ Letter
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摘要：

我们报告了ALMA观测到的[CI]（$^3P_1-^3P_0$），C $^{13}$ O，和CO $^{18}$（$J=1-0$）朝向附近的塞弗特星系NGC 613的中心区域。[CI]的$0.26"\times0.23"(=22\times20$ pc）和C $^{13}$ O和CO $^{18}$的$0.42"\times0.35"(=36\times30$ pc）具有非常高的分辨率，可分辨出环核盘（CND）和恒星形成环。[CI]在环中的分布类似于CO发射，尽管[CI]在CND中突出。这可能是由于CND中高温下的低光学深度导致的CO同位素的低强度造成的。我们发现[CI]与C-$^{12}$ O（3-2）（$R_{\rm CI/CO}$）和$^{13}$ O（1-0）（$R_{\rm CI/C^{13}O}$）的强度比在环边缘附近的几个位置处很高。CO谱线在环斑和高$R_{\rm CI/CO}$处的谱线轮廓基本一致，而[CI]在高$R_{\rm CI/CO}$处的谱线轮廓与CO谱线轮廓不同，这表明高$R_{\rm CI/CO}$处的[CI]与CO谱线所示踪的气体不同。NGC 613短轴方向的[CI]运动学可以解释为气泡状的分子外流。分子气体的流出速率大于恒星的形成速率。活动星系核主要通过射电喷流对气流进行助推。

英文摘要：

We report ALMA observations of [CI]($^3P_1-^3P_0$), C$^{13}$O, and CO$^{18}$ ($J=1-0$) toward the central region of a nearby Seyfert galaxy NGC 613. The very high resolutions of $0.26"\times0.23"(=22\times20$ pc) for [CI] and $0.42"\times0.35"(=36\times30$ pc) for C$^{13}$O, and CO$^{18}$ resolve the circum-nuclear disk (CND) and star-forming ring. The distribution of [CI] in the ring resembles that of the CO emission, although [CI] is prominent in the CND. This can be caused by the low intensities of the CO isotopes due to the low optical depths under the high temperature in the CND. We found that the intensity ratios of [CI] to C$^{12}$O(3-2) ($R_{\rm CI/CO}$) and to C$^{13}$O(1-0) ($R_{\rm CI/C^{13}O}$) are high at several positions around the edge of the ring. The spectral profiles of CO lines mostly correspond each other in the spots of the ring and high $R_{\rm CI/CO}$, but those of [CI] at spots of high $R_{\rm CI/CO}$ are different from CO. These results indicate that [CI] at the high $R_{\rm CI/CO}$ traces different gas from that traced by the CO lines. The [CI] kinematics along the minor axis of NGC 613 could be interpreted as a bubbly molecular outflow. The outflow rate of molecular gas is higher than star formation rate in the CND. The flow could be mainly boosted by the AGN through its radio jets.

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