论文标题
在天线星系（NGC 4038/ngc 4039）中形成的年轻大型群集B1由云云碰撞触发
The formation of the young massive cluster B1 in the Antennae galaxies (NGC 4038/NGC 4039) triggered by cloud-cloud collision
论文作者
论文摘要
天线星系是主要合并中的星爆。 Tsuge等。 （2020）表明，天线星系中的五个巨型分子复合物具有基于60 pc分辨率的ALMA档案数据的云云碰撞的特征。在目前的工作中，我们分析了使用ALMA获得的14 pc分辨率的新CO数据，向Super Star群集（SSC）B1分析，并确认两个云显示出互补的分布，并以$ \ sim $ 70 $ 70 PC以及它们之间的连接桥功能。 The complementary distribution shows a good correspondence with the theoretical collision model (Takahira et al. 2014), and indicates that SSC B1 having $\sim$10$^{6}$ $M$$_{\odot}$ was formed by the trigger of a cloud-cloud collision with a time scale of $\sim$1Myr, which is consistent with the cluster age. SSC B1可能是由$ \ sim $ 10 $^{7} $ $ $ M $$ _ {\ odot} $的分子气成形成的，其星形效率为$ \ sim $ 10％。我们确定了一些在形成其他簇的地方。详细的气体运动表明，加速气体中的出色反馈无效，而电离在以$ 30 pc的半径为$ \ sim周围的气体周围的气体中起作用。结果揭示了母体的细节，其中形成了与球形相似的质量的簇。
The Antennae Galaxies is one of the starbursts in major mergers. Tsuge et al. (2020) showed that the five giant molecular complexes in the Antennae Galaxies have signatures of cloud-cloud collisions based on the ALMA archival data at 60 pc resolution. In the present work we analyzed the new CO data toward the super star cluster (SSC) B1 at 14 pc resolution obtained with ALMA, and confirmed that two clouds show complementary distribution with a displacement of $\sim$70 pc as well as the connecting bridge features between them. The complementary distribution shows a good correspondence with the theoretical collision model (Takahira et al. 2014), and indicates that SSC B1 having $\sim$10$^{6}$ $M$$_{\odot}$ was formed by the trigger of a cloud-cloud collision with a time scale of $\sim$1Myr, which is consistent with the cluster age. It is likely that SSC B1 was formed from molecular gas of $\sim$10$^{7}$ $M$$_{\odot}$ with a star formation efficiency of $\sim$10 % in 1 Myr. We identified a few places where additional clusters are forming. Detailed gas motion indicates stellar feedback in accelerating gas is not effective, while ionization plays a role in evacuating the gas around the clusters at a $\sim$30-pc radius. The results have revealed the details of the parent gas where a cluster having mass similar to a globular is being formed.
