论文标题
银河中心弧中的云云碰撞
Cloud-Cloud Collision in the Galactic Center Arc
论文作者
论文摘要
我们根据调查观察结果对射手座的云云碰撞（CCC）站点进行了搜索，该位点使用了调查观测值，使用了C $^{32} $ s $ s $ j = 1-0 $和SIO $ $ $ V = 0〜J = 0〜J = 2-1 $发射线中的Nobeyama 45-m望远镜。我们发现，在银河中心弧（GCA）中，候选者在冲击的分子气中丰富。其中一个是M0.014-0.054，位于我们以前的Alma Mosaic观察的映射区域。我们探索了C $^{32} $ s $ j = 2-1 $，C $^{34} $ s $ j = 2-1 $，SIO $ v = 0〜J = 2-1 $，H $^$^{13} $^{13} $ j = 1-1-1-1-1-1 $ n $ n $ n，以及$ n，$ n $ n，y $ n，y $ n，y y $ n，以及线。 M0.014-0.054可能是由GCA的垂直分子丝（VP）与银河系经度沿银河经度的其他分子丝之间形成的。发现PV图上的这些碰撞细丝之间的桥接特征，这是CCC站点中预期的特征。我们还发现了M0.014-0.054中的连续紧凑型物体，它们在H42 $α$重组线中没有对应物。它们在SO发射线中被检测到，并且将是“热分子核（HMC）”。因为一个HMC的LTE质量大于病毒质量，因此在重力上是结合的。在CCS发射线中也检测到这一点。嵌入的恒星太年轻，无法将周围的分子云电离。 VP通过多磁场追踪。由于使用CF方法估计磁场的强度为$ \ sim m $高斯，因此支持副总裁，以防止碎片化。 M0.014-0.054的HMC中的恒星形成很可能是由稳定细丝之间的CCC引起的，这可能是SGramc中的一种常见机制。
We performed a search of cloud-cloud collision (CCC) sites in the Sagittarius A molecular cloud (SgrAMC) based on the survey observations using the Nobeyama 45-m telescope in the C$^{32}$S $J=1-0$ and SiO $v=0~J=2-1$ emission lines. We found candidates being 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 C$^{32}$S $J=2-1$, C$^{34}$S $J=2-1$, 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 (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$α$ recombination line. They are detected in the SO emission line, and would be "Hot Molecular Core (HMC)"s. Because the LTE 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 poloidal magnetic field. Because the strength of the magnetic field is estimated to be $\sim m$Gauss using the CF 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.
