论文标题
在双重AGN宿主中形成恒星：附近的分子和电离气体，发光红外合并，MRK 266
Forming Stars in a Dual AGN Host: Molecular and Ionized Gas in the Nearby, Luminous Infrared Merger, Mrk 266
论文作者
论文摘要
我们提出基于MRK 266（NGC 5256）的冷和离子气体测量值的星形速率，该系统由两个碰撞气体富含气的星系组成，每个星系均托有一个活跃的银河系核。使用$^{12} $ co（1-0）观察结果与毫米波天文学研究的组合阵列（CARMA），我们在中央区域中发现总h $ _2 $质量为$ 1.1 \ pm0.3 \ pm0.3 \ times10^{10} $ $ m_ \ $ m_ \ odot $，这会导致可能的未来$ 25 $ 25 $ pm10 yr $^{ - 1} $。借助加拿大 - 弗朗西 - 弗朗西·霍瓦伊望远镜上的傅立叶变换光谱仪（Sitelle），我们测量了集成的h $α$光度，并估计当今的星星形成率为$ 15 \ pm2 m_ \ odot $ yr $ yr $ yr $^{ - 1} $在系统的核心中（避免使用两个活动核）。这些结果证实，MRK 266是一种中间阶段合并，近期恒星形成率相对较高，并且足够的分子气体可以维持数亿年。与合并相关的流动气体可能触发了Starburst发作和两个AGN，但是两个星系组件不同：SW核周围的区域似乎比NE核更活跃，而NE核似乎相对安静。我们推测，这种差异可能起源于两个系统中星际介质的性质。
We present star formation rates based on cold and ionized gas measurements of Mrk 266 (NGC 5256), a system composed of two colliding gas-rich galaxies, each hosting an active galactic nucleus. Using $^{12}$CO (1-0) observations with the Combined Array for Research in Millimeter-Wave Astronomy (CARMA), we find a total H$_2$ mass in the central region of $1.1\pm0.3\times10^{10}$ $M_\odot$ which leads to a possible future star formation rate of $25\pm10 M_\odot$ yr$^{-1}$. With the Fourier Transform Spectrograph (SITELLE) on the Canada-France-Hawaii Telescope, we measure an integrated H$α$ luminosity and estimate a present-day star formation rate of $15\pm2 M_\odot$ yr$^{-1}$ in the core of the system (avoiding the two active nuclei). These results confirm that Mrk 266 is an intermediate stage merger with a relatively high recent star formation rate and enough molecular gas to sustain it for a few hundred million years. Inflowing gas associated with the merger may have triggered both the starburst episode and two AGN but the two galaxy components differ: the region around the SW nucleus appears to be more active than the NE nucleus, which seems relatively quiet. We speculate that this difference may originate in the properties of the interstellar medium in the two systems.
