MOLECULAR DEVELOPMENT IN THE LARGE MAGELLANIC CLOUD-猫眼课题宝

大麦哲伦云中的分子发育

DOI：

发表时间：

2015

期刊：

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作者：

K. Acharyya;E. Herbst

使用一个新的网络和一个新的模型，我们研究了大麦哲伦云（LMC）的稠密云的冷部分的化学复杂性。我们在1 × 105和5 × 105 cm-3之间改变氢数密度，对于每种密度，我们运行AV = 3、5和10的模型。然后，对于每个密度和视觉消光，我们在10和50 K之间以小的间隔改变颗粒温度，同时保持气体温度恒定在20 K。我们使用了基于各种观测和分析的气体与尘埃质量比，并对LMC的元素丰度进行了缩放，以便它们代表所谓的“低”金属丰度。我们发现，虽然大麦哲伦星系是贫金属的，但它仍然显示出丰富的化学成分;我们银河系气相中几乎所有主要的观测物种都应该可以使用当今的观测设施进行检测。我们比较了我们的模型结果与观察到的气相丰度在一些冷和密集的来源，并发现合理的大多数物种良好的协议。我们还发现，一些观察到的结果，特别是甲醇，更好地匹配，如果这些地区目前拥有较低的温度，或拥有他们在过去。最后，我们讨论了我们的模拟丰度为H2O冰相对于总氢，和CO2，CO，CH 3OH，和NH3冰相对于水冰，并比较我们的值与两个观察到的冰CO2和CO-在LMC的年轻恒星物体的前面检测。

Using a new network and a new model, we have studied chemical complexity in cold portions of dense clouds of the Large Magellanic Cloud (LMC). We varied the hydrogen number density between 1 × 105 and 5 × 105 cm−3 and, for each density, we ran models for AV = 3, 5, and 10. Then, for each density and visual extinction we varied the grain temperature between 10 and 50 K in small intervals, while keeping the gas temperature constant at 20 K. We used a gas-to-dust mass ratio based on a variety of observations and analyses, and scaled the elemental abundances of the LMC so that they are representative of so-called “low” metallic abundances. We found that although the LMC is metal-poor, it still shows a rich chemistry; almost all the major observed species in the gas phase of our Galaxy should be detectable using present-day observational facilities. We compared our model results with observed gas-phase abundances in some cold and dense sources, and found reasonably good agreement for most species. We also found that some observed results, especially for methanol, are better matched if these regions currently possess lower temperatures, or possessed them in the past. Finally, we discussed our simulated abundances for H2O ice with respect to total hydrogen, and CO2, CO, CH3OH, and NH3 ices with respect to water ice, and compared our values with those for two observed ices—CO2 and CO—detected in front of young stellar objects in the LMC.

SPITZER SURVEY OF THE LARGE MAGELLANIC CLOUD, SURVEYING THE AGENTS OF A GALAXY'S EVOLUTION (SAGE). IV. DUST PROPERTIES IN THE INTERSTELLAR MEDIUM

DOI： 10.1088/0004-6256/136/3/919

发表时间： 2005-06

期刊：

The Astronomical Journal

影响因子： --

作者：

M. Meixner;K. Gordon;R. Indebetouw;J. Hora;B. Whitney;R. Blum;W. Reach;J. Bernard;M. Meade;B. Babler;C. Engelbracht;B. For;K. Misselt;U. Vijh;C. Leitherer;M. Cohen;E. Churchwell;F. Boulanger;J. Frogel;Y. Fukui;J. Gallagher;V. Gorjian;J. Harris;D. Kelly;A. Kawamura;Soyoung Kim;W. Latter;S. Madden;Ciska Markwick-Kemper;A. Mizuno;N. Mizuno;J. Mould;A. Nota;M. Oey;K. Olsen;T. Onishi;R. Paladini;N. Panagia;P. Pérez-González;H. Shibai;Sato Shuji;Linda J. Smith;L. Staveley-Smith;A. Tielens;T. Ueta;S. V. Dyk;K. Volk;M. Werner;D. Zaritsky

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MOLECULAR DEVELOPMENT IN THE LARGE MAGELLANIC CLOUD

大麦哲伦云中的分子发育

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