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| molecules:ism:h2ccn [2019/10/23 17:03] – mueller | molecules:ism:h2ccn [2021/02/26 15:50] (current) – mueller |
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| **[[https://doi.org/10.1051/0004-6361:20078956|Detection of Circumstellar CH<sub>2</sub>CHCN, CH<sub>2</sub>CN, CH<sub>3</sub>CCH, and H<sub>2</sub>CS]]**\\ | **[[https://doi.org/10.1051/0004-6361:20078956|Detection of Circumstellar CH<sub>2</sub>CHCN, CH<sub>2</sub>CN, CH<sub>3</sub>CCH, and H<sub>2</sub>CS]]**\\ |
| //Astron. Astrophys.// **479**, 493–501 (2008). | //Astron. Astrophys.// **479**, 493–501 (2008). |
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| | C. Cabezas, Y. Endo, E. Roueff, N. Marcelino, M. Agúndez, B. Tercero, and J. Cernicharo\\ |
| | reported on the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202040210|Space and laboratory observation of the deuterated cyanomethyl radical HDCCN]]**\\ |
| | //Astron. Astrophys.// **646**, Art. No. L1 (2021).\\ |
| | The 2<sub>02</sub> − 1<sub>01</sub> transition near 37.49 GHz with fine and hyperfine structure splitting was detected toward TMC-1 using the Yebes 40 m radio telescope in the course of a molecular line survey. The derived H<sub>2</sub>CCN to HDCCN ratio is 20 ± 4, i.e., ~40 per H atom, quite normal for TMC-1. |
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| Contributor(s): H. S. P. Müller; 12, 2003; 07, 2011 | Contributor(s): H. S. P. Müller; 12, 2003; 07, 2011; 02, 2021 |
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