molecules:ism:hccn_etc

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molecules:ism:hccn_etc [2019/02/25 22:38] – external edit 127.0.0.1molecules:ism:hccn_etc [2019/10/22 16:39] (current) – mueller
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 The cyanomethylene radical HCCN was observed with the IRAM 30 m telescope in the outer part of the circumstellar shell of the carbon-rich late-type star CW Leo, also known as IRC +10216, by\\ The cyanomethylene radical HCCN was observed with the IRAM 30 m telescope in the outer part of the circumstellar shell of the carbon-rich late-type star CW Leo, also known as IRC +10216, by\\
 M. Guélin and J. Cernicharo,\\ M. Guélin and J. Cernicharo,\\
-**[[http://cdsads.u-strasbg.fr/abs/1991A%26A...244L..21G|Astronomical Detection of the HCCN Radical – Toward a New Family of Carbon-Chain Molecules ?]]**\\+**[[https://ui.adsabs.harvard.edu/abs/1991A%26A...244L..21G|Astronomical Detection of the HCCN Radical – Toward a New Family of Carbon-Chain Molecules ?]]**\\
 //Astron. Astrophys.// **244**, L21–L24 (1991).\\ //Astron. Astrophys.// **244**, L21–L24 (1991).\\
 9 fine structure components of 4 rotational transitions (//N// = 4 – 3 to 7 – 6) between 87 and 154 GHz were not or not significantly blended. A rotational temperature of 12±4 K was derived which was modified slightly to 15±2 K in the letter describing the detection of HC<sub>4</sub>N, see below.\\ 9 fine structure components of 4 rotational transitions (//N// = 4 – 3 to 7 – 6) between 87 and 154 GHz were not or not significantly blended. A rotational temperature of 12±4 K was derived which was modified slightly to 15±2 K in the letter describing the detection of HC<sub>4</sub>N, see below.\\
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 More recently, the detection of the next member, cyanoethynylmethylene, was also detected with the same instrument in the outer part of the circumstellar shell of CW Leo:\\ More recently, the detection of the next member, cyanoethynylmethylene, was also detected with the same instrument in the outer part of the circumstellar shell of CW Leo:\\
 J. Cernicharo, M. Guélin, and J. R. Pardo,\\ J. Cernicharo, M. Guélin, and J. R. Pardo,\\
-**[[http://dx.doi.org/10.1086/426439|Detection of the Linear Radical HC<sub>4</sub>N in IRC +10216]]**\\+**[[https://doi.org/10.1086/426439|Detection of the Linear Radical HC<sub>4</sub>N in IRC +10216]]**\\
 //Astrophys. J.// **615**, L145–L148 (2004).\\ //Astrophys. J.// **615**, L145–L148 (2004).\\
 12 fine structure components of 4 rotational transitions (//N// = 18 – 17 to 21 – 20) between 82 and 97 GHz were detected; 4 lines were partially blended. A rotational temperature of 25±4 K was derived, similar to that of HC<sub>3</sub>N in this source. 12 fine structure components of 4 rotational transitions (//N// = 18 – 17 to 21 – 20) between 82 and 97 GHz were detected; 4 lines were partially blended. A rotational temperature of 25±4 K was derived, similar to that of HC<sub>3</sub>N in this source.
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 Contributor(s): H. S. P. Müller; 11, 2004; 01, 2012 Contributor(s): H. S. P. Müller; 11, 2004; 01, 2012
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