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--- molecules:ism:hc7n [2019/10/24 09:48] – mueller
+++ molecules:ism:hc7n [2020/08/12 12:42] (current) – mueller
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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]]**\\
 //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 line survey 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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