论文标题
银河中心云之间相互作用的证据M0.10-0.08和M0.11-0.11
Evidence for an interaction between the Galactic Center clouds M0.10-0.08 and M0.11-0.11
论文作者
论文摘要
我们使用在K和KA频段（〜25和36 GHz）的非常大的阵列（〜2-3“; 〜0.1 pc）对银河中心云M0.10-0.08进行无线电观察。M0.10.10-0.08云位于一个复杂的环境中，位于一个复杂的环境附近，在银河中心无线电和辅助M0.11-11-11-11-11-11-11-11-11-11-11-11-11 morecult.11 morecult.11 morcull coull。是一个紧凑型分子云（〜3 PC），其中包含多个紧凑型分子核（5+； <0.4 PC），从以下分子中检测到M0.10-0.08的15个分子跃迁： M0.10-0.08具有超过400 K的亮度温度和31个Maser候选物，温度在100-400 K之间。我们使用NH3对气体进行运动学分析，并检测多个速度成分，该区域的大部分速度为51.5 km/s。 37.6 km/s。我们还以10.6 km/s的速度归因于M0.11-0.11云的延伸，这是气体运动学的分析。
We present high-resolution (~2-3"; ~0.1 pc) radio observations of the Galactic center cloud M0.10-0.08 using the Very Large Array at K and Ka band (~25 and 36 GHz). The M0.10-0.08 cloud is located in a complex environment near the Galactic center Radio Arc and the adjacent M0.11-0.11 molecular cloud. From our data, M0.10-0.08 appears to be a compact molecular cloud (~3 pc) that contains multiple compact molecular cores (5+; <0.4 pc). In this study we detect a total of 15 molecular transitions in M0.10-0.08 from the following molecules: NH3, HC3N, CH3OH, HC5N, CH3CN, and OCS. We have identified more than sixty 36 GHz CH3OH masers in M0.10-0.08 with brightness temperatures above 400 K and 31 maser candidates with temperatures between 100-400 K. We conduct a kinematic analysis of the gas using NH3 and detect multiple velocity components towards this region of the Galactic center. The bulk of the gas in this region has a velocity of 51.5 km/s (M0.10-0.08) with a lower velocity wing at 37.6 km/s. We also detect a relatively faint velocity component at 10.6 km/s that we attribute to being an extension of the M0.11-0.11 cloud. Analysis of the gas kinematics, combined with past X-ray fluorescence observations, suggests M0.10-0.08 and M0.11-0.11 are located in the same vicinity of the Galactic center and could be physically interacting.
