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arXiv 1609.03051astro-ph.GAastro-ph.SR
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13个银河系红外泡区的分子谱线

Molecular Lines of 13 Galactic Infrared Bubble Regions

Qing-zeng Yan, Ye Xu, Bo Zhang, Deng-rong Lu, Xi Chen, Zheng-hong Tang

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55 Pages, 32 figures. Accepted for publication in AJ
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摘要：

我们研究了分子云的物理性质和恒星形成过程中的红外气泡，本质上是扩大HII区域。我们进行了13个银河系红外气泡场的观测，其中包含18个气泡。观察到5个分子系，12 CO（J = 1 -0），13 CO（J=1-0），C18 O（J=1 -0），HCN（J=1-0）和HCO+（J=1-0），并使用几个公开可用的调查，GLIMPSE，MIPSGAL，ATLASGAL，BGPS，VGPS，MAGPIS和NVSS进行比较。我们发现这些气泡通常与分子云相连，其中大多数是巨大的。几个气泡区域显示速度梯度和广泛的移动的配置文件，这可能是由于气泡的膨胀。气泡内分子云的质量在100到19，000太阳质量之间，其动力学年龄约为0.3-3.7百万年，这考虑到了周围分子云的内部湍流压力。在所有18个气泡附近发现了团块，其中四个具有较大角尺寸的气泡附近的分子云显示出壳状形态，表明可能发生了收集和崩溃或辐射驱动的内爆过程。由于邻近分子云的污染，只有六个气泡区域适合寻找外流，我们发现其中四个有外流活动。三个气泡在其边界处显示超紧凑的HII区域，其中一个可能是其流出的原因。总共只有六个气泡显示附近的恒星形成活动，我们认为恒星形成过程可能已经被触发。

英文摘要：

We investigated the physical properties of molecular clouds and star formation processes around infrared bubbles which are essentially expanding HII regions. We performed observations of 13 galactic infrared bubble fields containing 18 bubbles. Five molecular lines, 12CO (J=1-0), 13CO (J=1-0), C18O(J=1-0), HCN (J=1-0), and HCO+ (J=1-0), were observed, and several publicly available surveys, GLIMPSE, MIPSGAL, ATLASGAL, BGPS, VGPS, MAGPIS, and NVSS, were used for comparison. We find that these bubbles are generally connected with molecular clouds, most of which are giant. Several bubble regions display velocity gradients and broad shifted profiles, which could be due to the expansion of bubbles. The masses of molecular clouds within bubbles range from 100 to 19,000 solar mass, and their dynamic ages are about 0.3-3.7 Myr, which takes into account the internal turbulence pressure of surrounding molecular clouds. Clumps are found in the vicinity of all 18 bubbles, and molecular clouds near four of these bubbles with larger angular sizes show shell-like morphologies, indicating that either collect-and-collapse or radiation-driven implosion processes may have occurred. Due to the contamination of adjacent molecular clouds, only six bubble regions are appropriate to search for outflows, and we find that four of them have outflow activities. Three bubbles display ultra-compact HII regions at their borders, and one of them is probably responsible for its outflow. In total, only six bubbles show star formation activities in the vicinity, and we suggest that star formation processes might have been triggered.

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