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molecules:ism:cyanopropargyl [2021/11/03 13:53] mueller |
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| **[[https://doi.org/10.1051/0004-6361/202142156|Discovery of Interstellar 3-Cyanopropargyl Radical, CH<sub>2</sub>CCCN]]**\\ | **[[https://doi.org/10.1051/0004-6361/202142156|Discovery of Interstellar 3-Cyanopropargyl Radical, CH<sub>2</sub>CCCN]]**\\ | ||
| //Astron. Astrophys.// **654**, Art. No. L9 (2021).\\ | //Astron. Astrophys.// **654**, Art. No. L9 (2021).\\ | ||
| + | //ortho//-CH<sub>2</sub>C<sub>3</sub>N was identified through three //a//-type transitions with //J// = 8 − 7 to 10 − 9 and //K<sub>a</sub>// = 0 in the course of a molecular line survey of the prototypical cold dark molecular cloud TMC-1 carried out with the Yebes 40 m radio telescope between 31.0 and 50.4 GHz. These transitions displayed partially resolved fine and hyperfine structure splitting; few components were blended by lines of other species. Also observed were four transitions of //para//-CH<sub>2</sub>C<sub>3</sub>N with //J// = 8 − 7 or 9 − 8 and //K<sub>a</sub>// = 1, which displayed well resolved fine structure splitting; some of these lines were also blended. A value of //T//<sub>rot</sub> = 7 ± 1 K was derived. The column density of CH<sub>2</sub>C<sub>3</sub>N is about a factor of 100 lower than that of CH<sub>2</sub>CN. And while CH<sub>2</sub>C<sub>3</sub>N is roughly a factor of 10 less abundant than CH<sub>3</sub>C<sub>3</sub>N, CH<sub>2</sub>CN is **more abundant** than CH<sub>3</sub>CN by a factor of about 3.\\ | ||
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| + | Contributor(s): H. S. P. Müller; 11, 2021 | ||
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