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| molecules:ism:hc9n [2020/08/12 12:39] – mueller | molecules:ism:hc9n [2026/07/29 14:58] (current) – mueller |
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| **[[https://ui.adsabs.harvard.edu/abs/1978ApJ...223L.105B|The Detection of HC<sub>9</sub>N in Interstellar Space]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1978ApJ...223L.105B|The Detection of HC<sub>9</sub>N in Interstellar Space]]**\\ |
| //Astrophys. J.// **223**, L105–L107 (1978)\\ | //Astrophys. J.// **223**, L105–L107 (1978)\\ |
| reported the first detection of this cyanopolyyne in two transitions (//J// = 18 – 17 and 25 – 24 near 10.5 and 14.5 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory before the molecules was detected in the laboratory. The spectroscopic parameters were estimated from the smaller cyanopolyynes. Heile's Cloud 2 is better known as TMC-1. | reported the first detection of this cyanopolyyne in two transitions (//J// = 18 – 17 and 25 – 24 near 10.5 and 14.5 GHz, respectively) in Heile's Cloud 2 employing the 46 m radio telecope of the Algonquin Radio Observatory before the molecules was detected in the laboratory. The spectroscopic parameters were estimated from the smaller cyanopolyynes. Heile's Cloud 2 is better known as TMC-1.\\ |
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| More recently, the molecule was also detected in six transitions in the circumstellar shell of the famous carbon star CW Leo:\\ | More recently, the molecule was also detected in six transitions in the circumstellar shell of the famous carbon star CW Leo:\\ |
| **[[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,\\ |
| //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\\ | 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\\ |
| **[[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]]**\\ | **[[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).\\ | //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>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.\\ | 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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| | J. R. Pardo, J. Cernicharo, J. P. Fonfría, C. Cabezas, M. Agúndez, B. Tercero, N. Marcelino, P. de Vicente, L. Velilla-Prieto and M. Guélin\\ |
| | announced some time later the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202659372|Discovery of HC<sub>9</sub>N //v//<sub>19</sub> Overtones in IRC +10216]]**\\ |
| | //Astron. Astrophys.// **709**, Art. No. L13 (2026).\\ |
| | Deeper integration than in the previous entry permitted overtone states of HC<sub>9</sub>N to detect up to //v//<sub>19</sub> = 8.\\ |
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| Contributor(s): H. S. P. Müller; 02, 2006; 06, 2009; 08, 2020. | Contributor(s): H. S. P. Müller; 02, 2006; 06, 2009; 08, 2020; 07, 2026. |
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