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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Cloud-cloud collision in the Galactic Center Arc
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Cloud-cloud collision in the Galactic Center Arc

机译：银河中心弧线的云云碰撞

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We performed a search of cloud-cloud collision (CCC) sites in the Sagittarius A molecular cloud (SgrAMC) based on the survey observations using the Nobeyama 45 m telescope in the (CS)-S-32 J = 1-0 and SiO v = 0 J = 2-1 emission lines. We found candidates abundant in shocked molecular gas in the Galactic Center Arc (GCA). One of them, M0.014-0.054, is located in the mapping area of our previous ALMA mosaic observation. We explored the structure and kinematics of M0.014-0.054 in the (CS)-S-32 J = 2-1, (CS)-S-34 J = 2-1, SiO v = 0 J = 2-1, H(13)CO(+)J = 1-0, and SO N, J = 2, 2-1, 1 emission lines and fainter emission lines. M0.014-0.054 is likely formed by the CCC between the vertical molecular filaments (the "vertical part," or VP) of the GCA, and other molecular filaments along Galactic longitude. The bridging features between these colliding filaments on the PV diagram are found, which are the characteristics expected in CCC sites. We also found continuum compact objects in M0.014-0.054, which have no counterpart in the H42 alpha recombination line. They are detected in the SO emission line, and would be "hot molecular cores" (HMCs). Because the local thermodynamic equilibrium mass of one HMC is larger than the virial mass, it is bound gravitationally. This is also detected in the CCS emission line. The embedded star would be too young to ionize the surrounding molecular cloud. The VP is traced by a poloidal magnetic field. Because the strength of the magnetic field is estimated to be similar to mgauss using the Chandrasekhar-Fermi method, the VP is supported against fragmentation. The star formation in the HMC of M0.014-0.054 is likely induced by the CCC between the stable filaments, which may be a common mechanism in the SgrAMC.
机译：我们根据在（CS）-S-32 J=1-0和SiO v=0 J=2-1发射线上使用Nobeyama 45米望远镜进行的观测，对人马座a分子云（SgrAMC）中的云-云碰撞（CCC）位置进行了搜索。我们在星系中心弧（GCA）中发现了大量的受冲击分子气体。其中一个，M0。014-0.054，位于我们之前阿尔玛马赛克观测的绘图区域。我们探索了M0的结构和运动学。014-0.054在（CS）-S-32J=2-1，（CS）-S-34J=2-1，SiO v=0J=2-1，H（13）CO（+）J=1-0，所以N，J=2，2-1，1发射线和较暗的发射线。M0。014-0.054可能是由GCA的垂直分子细丝（垂直部分，或VP）和沿银河经度的其他分子细丝之间的CCC形成的。在PV图上发现了这些碰撞灯丝之间的桥接特征，这是CCC站点预期的特征。我们还在M0中发现了连续致密的物体。014-0.054，在H42α重组系中没有对应物。它们在SO发射线上被探测到，将成为“热分子核”（HMC）。因为一个HMC的局部热力学平衡质量大于维里质量，所以它是引力束缚的。这也在CCS排放管线中检测到。嵌入的恒星太年轻，无法电离周围的分子云。VP由极向磁场追踪。由于使用钱德拉塞哈尔费米方法估计磁场强度与MGAUS相似，因此VP可以防止碎裂。M0的HMC中的恒星形成。014-0.054可能是由稳定丝之间的CCC诱导的，这可能是SgrAMC中的常见机制。

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