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molecules:ism:sh-plus [2019/10/18 13:12] – mueller | molecules:ism:sh-plus [2021/07/14 10:58] (current) – mueller | ||
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**[[https:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | The absorption originates not only from the envelope of Sgr B2(M), but also from various spiral arm molecular clouds along the line of sight. The observation of the stronger //J// = 2 – 1 fine structure component of the same rotational transition near 526 GHz from ground is hampered by a strong terrestrial water line, but it can be observed from satellites such as // | + | The absorption originates not only from the envelope of Sgr B2(M), but also from various spiral arm molecular clouds along the line of sight. The observation of the stronger //J// = 2 – 1 fine structure component of the same rotational transition near 526 GHz from ground is hampered by a strong terrestrial water line, but it can be observed from satellites such as // |
Shortly thereafter, SH< | Shortly thereafter, SH< | ||
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**[[https:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | Note that the article actually appeared before the one mentioned above. | + | Note that the article actually appeared before the one mentioned above.\\ |
B. Godard, E. Falgarone, M. Gerin, D. C. Lis, M. De Luca, J. H. Black, J. R. Goicoechea, J. Cernicharo, D. A. Neufeld, K. M. Menten, and M. Emprechtinger, | B. Godard, E. Falgarone, M. Gerin, D. C. Lis, M. De Luca, J. H. Black, J. R. Goicoechea, J. Cernicharo, D. A. Neufeld, K. M. Menten, and M. Emprechtinger, | ||
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**[[https:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | The 525 GHz FS component of SH< | + | The 525 GHz FS component of SH< |
Z. Nagy, F. F. S. van der Tak, V. Ossenkopf, M. Gerin, F. Le Petit, J. Le Bourlot, J. H. Black, J. R. Goicoechea, C. Joblin, M. Röllig, and E. A. Bergin,\\ | Z. Nagy, F. F. S. van der Tak, V. Ossenkopf, M. Gerin, F. Le Petit, J. Le Bourlot, J. H. Black, J. R. Goicoechea, C. Joblin, M. Röllig, and E. A. Bergin,\\ | ||
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The effect of high electron density and vibrationally excited H< | The effect of high electron density and vibrationally excited H< | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | As for other hydrides, such as CH< | + | As for other hydrides, such as CH< |
+ | |||
+ | T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, | ||
+ | described\\ | ||
+ | **[[https:// | ||
+ | //Astron. Astrophys.// | ||
+ | They observed the //J// = 2 − 1 and 1 − 1 fine structure components of the //N// = 1 − 0 rotational transition of < | ||
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- | Contributor(s): | + | Contributor(s): |
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