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| L. W. Avery, N. W. Broten, J. M. McLeod, T. Oka, and H. W. Kroto\\ | L. W. Avery, N. W. Broten, J. M. McLeod, T. Oka, and H. W. Kroto\\ |
| reported on the\\ | reported on the\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1976ApJ...205L.173A|Detection of the Heavy Interstellar Molecule Cyanodiacetylene]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1976ApJ...205L.173A|Detection of the Heavy Interstellar Molecule Cyanodiacetylene]]**\\ |
| //Astrophys. J.// **205**, L173–L175 (1976).\\ | //Astrophys. J.// **205**, L173–L175 (1976).\\ |
| The //J// = 4 – 3 transition near 10.651 GHz was observed in emission toward Sagittarius (Sgr) B2 employing the 46 m radio telecope of the Algonquin Radio Observatory. | The //J// = 4 – 3 transition near 10.651 GHz was observed in emission toward Sagittarius (Sgr) B2 employing the 46 m radio telecope of the Algonquin Radio Observatory. |
| N. W. Broten, J. M. McLeod, T. Oka, L. W. Avery, J. W. Brooks, R. X. McGee, and L. M. Newton\\ | N. W. Broten, J. M. McLeod, T. Oka, L. W. Avery, J. W. Brooks, R. X. McGee, and L. M. Newton\\ |
| reported subsequently on\\ | reported subsequently on\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1976ApJ...209L.143B|Evidence for Weak Maser Action in Interstellar Cyanodiacetylene]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1976ApJ...209L.143B|Evidence for Weak Maser Action in Interstellar Cyanodiacetylene]]**\\ |
| //Astrophys. J.// **209**, L143–L147 (1976).\\ | //Astrophys. J.// **209**, L143–L147 (1976).\\ |
| The //J// = 8 – 7 transition near 21.301 GHz was observed toward Sagittarius /Sgr) B2 employing the 46 m radio telecope of the Algonquin Radio Observatory. In addition, the Parkes 64 m dish was used to study the The //J// = 1 – 0 transition near 2.663 GHz with well-resolved hyperfine structure. The high intensity of the latter emission lines were viewed as evidence for weak maser activity. | The //J// = 8 – 7 transition near 21.301 GHz was observed toward Sagittarius /Sgr) B2 employing the 46 m radio telecope of the Algonquin Radio Observatory. In addition, the Parkes 64 m dish was used to study the The //J// = 1 – 0 transition near 2.663 GHz with well-resolved hyperfine structure. The high intensity of the latter emission lines were viewed as evidence for weak maser activity. |
| 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// = 9 – 8 transition near 23.964 GHz was detected for the smaller polyyne.\\ | The //J// = 9 – 8 transition near 23.964 GHz was detected for the smaller polyyne.\\ |
| The detection of DC<sub>5</sub>N in TMC-1 was reported by two groups simultaneously:\\ | The detection of DC<sub>5</sub>N in TMC-1 was reported by two groups simultaneously:\\ |
| J. M. MacLeod, L. W. Avery, and N. W. Broten,\\ | J. M. MacLeod, L. W. Avery, and N. W. Broten,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1981ApJ...251L..33M|//Astrophys. J.//]] 251**, L33–L36 (1981); and\\ | **[[https://ui.adsabs.harvard.edu/abs/1981ApJ...251L..33M|//Astrophys. J.//]] 251**, L33–L36 (1981); and\\ |
| F. P. Schloerb, R. L. Snell, W. D. Langer, and J. S. Young,\\ | F. P. Schloerb, R. L. Snell, W. D. Langer, and J. S. Young,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1981ApJ...251L..37S|//Astrophys. J.//]] 251**, L37–L41 (1981).\\ | **[[http://cdsads.u-strasbg.fr/abs/1981ApJ...251L..37S|//Astrophys. J.//]] 251**, L37–L41 (1981).\\ |
| S. Takano, H. Suzuki, M. Ohishi, S.-I. Ishikawa, N. Kaifu, Y. Hirahara, and A. Masuda\\ | S. Takano, H. Suzuki, M. Ohishi, S.-I. Ishikawa, N. Kaifu, Y. Hirahara, and A. Masuda\\ |
| used the Nobeyama 45 m telescope for the\\ | used the Nobeyama 45 m telescope for the\\ |
| **[[http://adsabs.harvard.edu/abs/1990ApJ...361L..15T|Detection of Five <sup>13</sup>C Isotopic Species of HC<sub>5</sub>N in TMC-1]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1990ApJ...361L..15T|Detection of Five <sup>13</sup>C Isotopic Species of HC<sub>5</sub>N in TMC-1]]**\\ |
| //Astrophys. J.// **361**, L15–L18 (1990).\\ | //Astrophys. J.// **361**, L15–L18 (1990).\\ |
| The //J// = 14 – 13 transitions bewteen 36 and 38 GHz were detected at intensities compatible with the <sup>12</sup>C/<sup>13</sup>C ratio in the solar neighborhood. | The //J// = 14 – 13 transitions bewteen 36 and 38 GHz were detected at intensities compatible with the <sup>12</sup>C/<sup>13</sup>C ratio in the solar neighborhood. |
| **[[https://doi.org/10.1086/430774|Observational Evidence of the Formation of Cyanopolyynes in CRL 618 through the Polymerization of HCN]]**\\ | **[[https://doi.org/10.1086/430774|Observational Evidence of the Formation of Cyanopolyynes in CRL 618 through the Polymerization of HCN]]**\\ |
| //Astrophys. J.// **628**, 275–282 (2005).\\ | //Astrophys. J.// **628**, 275–282 (2005).\\ |
| Four low-lying states (//v//<sub>11</sub> = 1 to 3 and //v//<sub>10</sub> = 1) were detected with vibrational energies of up to about 315 <sup>–1</sup>. | Four low-lying states (//v//<sub>11</sub> = 1 to 3 and //v//<sub>10</sub> = 1) were detected with vibrational energies of up to about 315 cm<sup>–1</sup>. |
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| Contributor(s): H. S. P. Müller; 01, 2018. | Contributor(s): H. S. P. Müller; 01, 2018. |
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