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molecules:ism:cyanopropargyl [2021/11/03 14:08]
mueller
molecules:ism:cyanopropargyl [2021/11/03 14:14] (current)
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 ten lower than that of CH<​sub>​2</​sub>​CN. ​+//​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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