Ammonia observations towards the Aquila Rift cloud complex
Ammonia observations towards the Aquila Rift cloud complex
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对天鹰裂谷云复合体的氨观测
DOI：
10.1051/0004-6361/202037659
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发表时间：
2020
影响因子：
6.5
通讯作者：
Sailanbek Serikbek
中科院分区：
文献类型：
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作者：
Tursun Kadirya;Esimbek Jarken;Henkel Christian;Tang Xindi;Wu Gang;Li Dalei;Zhou Jianjun;He Yuxin;Komesh Toktarkhan;Sailanbek Serikbek
我们利用南山26米望远镜对天鹰座裂谷复合体进行了观测，包括NH3（1，1）和（2，2）过渡区的巨蛇座南部和W 40区域。我们的观测范围约为1.5° × 2.2°（11.4 pc × 16.7 pc）。由NH3（2，2）/（1，1）比值得到的天鹰座裂谷复合体中致密气体的动力学温度范围为8.9 ~ 35.0 K，平均值为15.3 ± 6.1 K（误差为平均值的标准差）。低气体温度与Serpens South相关，范围为8.9至16.8 K，平均值为12.3 ± 1.7 K，而W 40区域的致密气体显示出更高的温度，范围为17.7至35.0 K，平均值为25.1 ± 4.9 K。动力学温度从para-NH 3（2，2）/（1，1）对HiGal尘埃温度的比较表明，气体和尘埃温度是一致的低质量星星形成区域的巨蛇座南。在高质量星星形成区W 40中，测得的气体动力学温度高于尘埃的温度。NH_3（1，1）速度弥散的湍流分量与气体动力学温度呈正相关，这表明稠密气体可能是通过耗散湍流能量而被加热的。对于通过与代表尘埃排放的赫歇尔红外连续谱数据比较获得的总-NH3（帕拉+邻位）丰度分数，我们发现值从0.1 ×10− 8到2.1 ×10− 7，平均值为6.9（±4.5）× 10−8。巨蛇座南蛇座的总NH3（帕拉+邻位）丰度从0.2 ×10− 8到2.1 ×10− 7不等，平均值为8.6（±3.8）× 10−8。在W 40中，数值较低，介于0.1和4.3 ×10− 8之间，平均值为1.6（±1.4）× 10−8。弱的速度梯度表明，转动能是引力能的一个可忽略的部分。在W 40中，气体和尘埃的温度并不强烈地依赖于最近形成的大质量恒星的投影距离。总的来说，映射区域的形态是环状的，在较低的银河系边缘有较强的发射，在较高的银河系边缘有较弱的发射。然而，这两个部分之间是否存在物理连接仍然值得怀疑。
We surveyed the Aquila Rift complex including the Serpens South and W 40 regions in the NH3(1,1) and (2,2) transitions making use of the Nanshan 26-m telescope. Our observations cover an area of ~ 1.5° × 2.2° (11.4 pc × 16.7 pc). The kinetic temperatures of the dense gas in the Aquila Rift complex obtained from NH3(2,2)/(1,1) ratios range from 8.9 to 35.0 K with an average of 15.3 ± 6.1 K (errors are standard deviations of the mean). Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 ± 1.7 K, while dense gas in the W 40 region shows higher temperatures ranging from 17.7 to 35.0 K with an average of 25.1 ± 4.9 K. A comparison of kinetic temperatures derived from para-NH3(2,2)/(1,1) against HiGal dust temperatures indicates that the gas and dust temperatures are in agreement in the low-mass-star formation region of Serpens South. In the high-mass-star formation region W 40, the measured gas kinetic temperatures are higher than those of the dust. The turbulent component of the velocity dispersion of NH3(1,1) is found to be positively correlated with the gas kinetic temperature, which indicates that the dense gas may be heated by dissipation of turbulent energy. For the fractional total-NH3(para+ortho) abundance obtained by a comparison withHerschelinfrared continuum data representing dust emission, we find values from 0.1 ×10−8to 2.1 ×10−7with an average of 6.9 (±4.5) × 10−8. Serpens South also shows a fractional total-NH3(para+ortho) abundance ranging from 0.2 ×10−8to 2.1 ×10−7with an average of 8.6 (±3.8) × 10−8. In W 40, values are lower, between 0.1 and 4.3 ×10−8with an average of 1.6 (±1.4) × 10−8. Weak velocity gradients demonstrate that the rotational energy is a negligible fraction of the gravitational energy. In W 40, gas and dust temperatures are not strongly dependent on the projected distance to the recently formed massive stars. Overall, the morphology of the mapped region is ring-like, with strong emission at lower and weak emission at higher Galactic longitudes. However, the presence of a physical connection between the two parts remains questionable.