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molecules:ism:hc7n [2019/04/25 13:39]
mueller
molecules:ism:hc7n [2020/08/12 12:36]
mueller
Line 2: Line 2:
  
 H. W. Kroto, C. Kirby, D. R. M. Walton, L. W. Avery, N. W. Broten, J. M. MacLeod, and T. Oka,\\ H. W. Kroto, C. Kirby, D. R. M. Walton, L. W. Avery, N. W. Broten, J. M. MacLeod, and T. Oka,\\
-**[[http://cdsads.u-strasbg.fr/​abs/​1978ApJ...219L.133K|The Detection of Cyanohexatriyne,​ H(C≡C)<​sub>​3</​sub>​CN,​ in Heile'​s Cloud 2]]**\\+**[[https://ui.adsabs.harvard.edu/​abs/​1978ApJ...219L.133K|The Detection of Cyanohexatriyne,​ H(C≡C)<​sub>​3</​sub>​CN,​ in Heile'​s Cloud 2]]**\\
 //​Astrophys. J.// **219**, L133–L137 (1978)\\ //​Astrophys. J.// **219**, L133–L137 (1978)\\
 reported the first detection of this cyanopolyyne in two transitions (//​J//​ = 9 – 8 and 21 – 20 near 10.15 and 23.69 GHz, respectively) in Heile'​s Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory. reported the first detection of this cyanopolyyne in two transitions (//​J//​ = 9 – 8 and 21 – 20 near 10.15 and 23.69 GHz, respectively) in Heile'​s Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory.
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 More recently, the Effelsberg 100 m telecope was used to study the circumstellar shell of the famous carbon star CW Leo:\\ More recently, the Effelsberg 100 m telecope was used to study the circumstellar shell of the famous carbon star CW Leo:\\
 G. Winnewisser and C. M. Walmsley,\\ G. Winnewisser and C. M. Walmsley,\\
-**[[http://cdsads.u-strasbg.fr/​abs/​1978A%26A....70L..37W|The Detection of HC<​sub>​5</​sub>​N and HC<​sub>​7</​sub>​N in IRC +10216]]**\\+**[[https://ui.adsabs.harvard.edu/​abs/​1978A%26A....70L..37W|The Detection of HC<​sub>​5</​sub>​N and HC<​sub>​7</​sub>​N in IRC +10216]]**\\
 //Astron. Astrophys.//​ **70**, L37–L39 (1978).\\ //Astron. Astrophys.//​ **70**, L37–L39 (1978).\\
 The //​J//​ = 21 – 10 transition near 23.688 GHz was detected for the larger polyyne. The //​J//​ = 21 – 10 transition near 23.688 GHz was detected for the larger polyyne.
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 The molecule has also been detected with the Effelsberg 100 m telescope in the circumstellar envelope of the carbon-rich post-AGB star V1610 Cyg, which is somewhat better known as CRL 2688, by\\ The molecule has also been detected with the Effelsberg 100 m telescope in the circumstellar envelope of the carbon-rich post-AGB star V1610 Cyg, which is somewhat better known as CRL 2688, by\\
 Nguyen-Q-Rieu,​ D. Graham, and V. Bujarrabal,​\\ Nguyen-Q-Rieu,​ D. Graham, and V. Bujarrabal,​\\
-**[[http://cdsads.u-strasbg.fr/​abs/​1984A%26A...138L...5N|Ammonia and Cyanotriacetylene in the Envelopes of CRL 2688 and IRC +10216]]**\\+**[[https://ui.adsabs.harvard.edu/​abs/​1984A%26A...138L...5N|Ammonia and Cyanotriacetylene in the Envelopes of CRL 2688 and IRC +10216]]**\\
 //Astron. Astrophys.//​ **138**, L5–L8 (1984). //Astron. Astrophys.//​ **138**, L5–L8 (1984).
  
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 **[[https://​doi.org/​10.1093/​mnras/​stx2972|Detection of HC<​sub>​5</​sub>​N and HC<​sub>​7</​sub>​N Isotopologues in TMC-1 with the Green Bank Telescope]]**\\ **[[https://​doi.org/​10.1093/​mnras/​stx2972|Detection of HC<​sub>​5</​sub>​N and HC<​sub>​7</​sub>​N Isotopologues in TMC-1 with the Green Bank Telescope]]**\\
 //Mon. Not. R. Astron. Soc.// **474**, 5068–5075 (2018); by\\ //Mon. Not. R. Astron. Soc.// **474**, 5068–5075 (2018); by\\
-A. M. Burkhardt, E. Herbst, S. V. Kalenskii, M. C. McCarthy, A. J. Remijan, and B. A. McGuire.+A. M. Burkhardt, E. Herbst, S. V. Kalenskii, M. C. McCarthy, A. J. Remijan, and B. A. McGuire.\\
  
 +J. R. Pardo, C. Bermúdez, C. Cabezas, M. Agúndez, J. D. Gallego, J. P. Fonfría, L. Velilla-Prieto,​ G. Quintana-Lacaci,​ B. Tercero, M. Guélin, and J. Cernicharo\\
 +reported on the\\
 +**[[https://​doi.org/​10.1051/​0004-6361/​202038571|Detection of Vibrationally Excited HC<​sub>​7</​sub>​N and HC<​sub>​9</​sub>​N in IRC +10216]]**\\
 +//Astron. Astrophys.//​ **640**, Art. No. L13 (2020).\\
 +The authors carried out an unbiased molecular with the Yebes 40 m dish between 31 and 50 GHz toward the circumstellar envelope of the famous C-rich AGB star CW Leonis. Numerous transitions of HC<​sub>​7</​sub>​N in its lowest excited state //​v//<​sub>​15</​sub>​ = 1 were detected despite a rotational temperature of around 25 K. The derived HC<​sub>​5</​sub>​N to HC<​sub>​7</​sub>​N ratio is extremely low, roughly 2.4. The derived HC<​sub>​7</​sub>​N to HC<​sub>​9</​sub>​N ratio is still very low, roughly 7.7.\\
  
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-Contributor(s):​ H. S. P. Müller; 04, 2012; 01, 2018.+----
  
 +Contributor(s):​ H. S. P. Müller; 04, 2012; 01, 2018; 08, 2020.
  
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  • molecules/ism/hc7n.txt
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