We present high-frequency Karl G. Jansky Very Large Array (VLA) continuum and spectral line (NH3, H64α, and H63α) observations of the Galactic Center?Radio Arc region, covering the Sickle H ii region, the Quintuplet cluster, and molecular clouds M0.20?0.033?and M0.10?0.08. These observations show that the two velocity components of M0.20?0.033?(~25 and 80 km s?1), previously thought to be separate clouds along the same line-of-sight, are physically connected in position–velocity?space via a third southern component around 50 km s?1. Further position–velocity?analysis of the surrounding region, using lower-resolution survey observations taken with the Mopra and ATCA telescopes, indicates that both molecular components in M0.20?0.033?are physically connected to the M0.10?0.08?molecular cloud, which is suggested to be located on stream 1 in the Kruijssen et al. orbital model. The morphology and kinematics of the molecular gas in M0.20?0.033?indicate that the two velocity components in M0.20?0.033?constitute an expanding shell. Our observations suggest that the M0.20?0.033 expanding shell?has an expansion velocity of 40 km s?1,?with a systemic velocity of 53 km s?1, comparable to velocities detected in M0.10?0.08. The origin of the expanding shell is located near the Quintuplet cluster, suggesting that the energy and momentum output from this massive stellar cluster may have contributed to the expansion.
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机译：我们展示了银河中心？射电弧区域的高频卡尔·詹斯基超大阵列（VLA）连续谱和光谱线（NH3，H64α和H63α）观测结果，涵盖了镰刀H ii区域，五重星团和分子云M0.20？0.033？和M0.10？0.08。这些观察结果表明，M0.20？0.033？（〜25和80 km s？1）的两个速度分量以前被认为是沿着同一视线的分离云，它们在位置-速度-空间中物理相连。通过南部约50公里s？1的第三部分。使用Mopra和ATCA望远镜进行的低分辨率调查观察，进一步对周围区域进行位置-速度分析，表明M0.20？0.033？中的两个分子成分都与M0.10？0.08？分子云物理连接。 ，建议将其放置在Kruijssen等人的流1中。轨道模型。 M0.20≤0.033′中分子气体的形态学和运动学表明，M0.20≤0.033′中的两个速度分量构成了膨胀壳。我们的观察结果表明，M0.20〜0.033膨胀壳的膨胀速度为40 km s？1，系统速度为53 km s？1，与M0.10？0.08的速度相当。膨胀壳的起源位于五重星团附近，这表明这个巨大的恒星团的能量和动量输出可能对膨胀起到了作用。
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