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| molecules:ism:hc9n [2019/10/24 09:55] – mueller | molecules:ism:hc9n [2020/08/12 12:43] (current) – mueller |
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| M. B. Bell, L. W. Avery, J. M. MacLeod, and H. E. Matthews,\\ | M. B. Bell, L. W. Avery, J. M. MacLeod, and H. E. Matthews,\\ |
| **[[https://ui.adsabs.harvard.edu/abs/1992ApJ...400..551B|The Excitation Temperature of HC<sub>9</sub>N in the Circumstellar Envelope of IRC +10216]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1992ApJ...400..551B|The Excitation Temperature of HC<sub>9</sub>N in the Circumstellar Envelope of IRC +10216]]**\\ |
| //Astrophys. J.// **400**, 551–555 (1992). | //Astrophys. J.// **400**, 551–555 (1992).\\ |
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| Truong-Bach, D. Graham, and Nguyen-Q-Rieu,\\ | Truong-Bach, D. Graham, and Nguyen-Q-Rieu,\\ |
| **[[https://ui.adsabs.harvard.edu/abs/1993A%26A...277..133T|HC<sub>9</sub>N from the Envelopes of IRC +10216 and CRL 2688]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1993A%26A...277..133T|HC<sub>9</sub>N from the Envelopes of IRC +10216 and CRL 2688]]**\\ |
| //Astron. Astrophys.// **277**, 133–138 (1993);\\ | //Astron. Astrophys.// **277**, 133–138 (1993);\\ |
| detected one additional higher-//J// transition toward the former source and the same transition in a protoplanetary nebula. | detected one additional higher-//J// transition toward the former source and the same transition in a protoplanetary nebula.\\ |
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| | 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>9</sub>N in its lowest excited state //v//<sub>19</sub> = 1 were detected despite the low rotational temperature. The lines could be assigned unambiguously although no laboratory data were available for this excited state. 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; 02, 2006; 06, 2009. | Contributor(s): H. S. P. Müller; 02, 2006; 06, 2009; 08, 2020. |
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