Recent Updates to the Gas-phase Chemical Reactions and Molecular Lines in CLOUDY: Their Effects on Millimeter and Submillimeter Molecular Line Predictions
Recent Updates to the Gas-phase Chemical Reactions and Molecular Lines in CLOUDY: Their Effects on Millimeter and Submillimeter Molecular Line Predictions
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DOI：
10.3847/1538-4357/ac7789
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发表时间：
2022-06
期刊：
影响因子：
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通讯作者：
G. Shaw;G. Ferland;M. Chatzikos
中科院分区：
文献类型：
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作者：
G. Shaw;G. Ferland;M. Chatzikos
在这里，我们提出了我们目前的更新的气相化学反应速率和分子线的光谱合成代码多云，其影响的光谱建模的各种天体物理环境。我们包括HF，CF+，HC 3 N，ArH+，HCl，HCN，CN，CH和CH 2的能级，辐射和碰撞率。同时，我们扩展了涉及这些分子的分子网络。为此，我们增加了561个新反应，并更新了涉及这些分子的现有165个分子反应速率。结果，多云现在预测了这九个分子产生的所有谱线。此外，我们还更新H2-H2碰撞数据旋转水平J = 31 v = 0。我们展示了光谱模拟这些分子的一些天体物理环境。我们现有的蟹状星云球状体模型成功地预测了所观察到的ArH+柱密度。我们的模型预测了蟹状星云中可检测到的HeH+、OH+和CH+。我们还模拟了HD 185418，W31 C和NGC 253的星际介质，我们的预测与观测到的误差条内的大多数观测到的柱密度相匹配。分子谱线经常跟踪各种物理条件。因此，这一更新将非常支持各种天体物理环境的光谱建模，特别是分别使用阿塔卡玛大型毫米/亚毫米阵列和詹姆斯韦伯太空望远镜进行亚毫米和中红外观测。
Here, we present our current updates to the gas-phase chemical reaction rates and molecular lines in the spectral synthesis code cloudy, and its implications in spectroscopic modeling of various astrophysical environments. We include energy levels, and radiative and collisional rates for HF, CF+, HC3N, ArH+, HCl, HCN, CN, CH, and CH2. Simultaneously, we expand our molecular network involving these molecules. For this purpose, we have added 561 new reactions and have updated the existing 165 molecular reaction rates involving these molecules. As a result, cloudy now predicts all the lines arising from these nine molecules. In addition, we also update H2–H2 collisional data up to rotational levels J = 31 for v = 0. We demonstrate spectroscopic simulations of these molecules for a few astrophysical environments. Our existing model for globules in the Crab Nebula successfully predicts the observed column density of ArH+. Our model predicts a detectable amount of HeH+, OH+, and CH+ for the Crab Nebula. We also model the interstellar medium toward HD185418, W31C, and NGC 253, and our predictions match with most of the observed column densities within the observed error bars. Very often molecular lines trace various physical conditions. Hence, this update will be very supportive for spectroscopic modeling of various astrophysical environments, particularly involving submillimeter and mid-infrared observations using the Atacama Large Millimeter/submillimeter Array and the James Webb Space Telescope, respectively.