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| molecules:ism:c-c3h [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:c-c3h [2019/10/22 16:35] (current) – mueller |
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| C<sub>3</sub>H exists in two isomeric forms, a linear one and a cyclic one. The latter is considerably higher in energy. Still, both seem to be equally abundant in cold dark clouds. The cyclic isomer has three CC bonds of essentially equal lengths which correspond to a bond order of 1.5. The molecule can be viewed best as derived from cyclopropane by removing 2 × 2 plus one H atoms, yielding cyclopropanediylidenyl as the probably most appropriate name. //c//-C<sub>3</sub>H was detected first in the dense cold molecular cloud TMC-1 by\\ | C<sub>3</sub>H exists in two isomeric forms, a linear one and a cyclic one. The latter is considerably higher in energy. Still, both seem to be equally abundant in cold dark clouds. The cyclic isomer has three CC bonds of essentially equal lengths which correspond to a bond order of 1.5. The molecule can be viewed best as derived from cyclopropane by removing 2 × 2 plus one H atoms, yielding cyclopropanediylidenyl as the probably most appropriate name. //c//-C<sub>3</sub>H was detected first in the dense cold molecular cloud TMC-1 by\\ |
| S. Yamamoto, S. Saito, M. Ohishi, H. Suzuki, S.-I. Ishikawa, N. Kaifu, and A. Murakami,\\ | S. Yamamoto, S. Saito, M. Ohishi, H. Suzuki, S.-I. Ishikawa, N. Kaifu, and A. Murakami,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1987ApJ...322L..55Y|Laboratory and Astronomical Detection of the Cyclic C<sub>3</sub>H Radical]]**,\\ | **[[https://ui.adsabs.harvard.edu/abs/1987ApJ...322L..55Y|Laboratory and Astronomical Detection of the Cyclic C<sub>3</sub>H Radical]]**,\\ |
| //Astrophys. J.// **322**, L55–L58 (1987).\\ | //Astrophys. J.// **322**, L55–L58 (1987).\\ |
| Two hyperfine components each were detected for the two fine structure components of the 2<sub>12</sub> – 1<sub>11</sub> transition near 91.5 and 91.7 GHZ, respectively, employing the Nobeyama 45 m telescope. | Two hyperfine components each were detected for the two fine structure components of the 2<sub>12</sub> – 1<sub>11</sub> transition near 91.5 and 91.7 GHZ, respectively, employing the Nobeyama 45 m telescope. |
| Two hfs components of the 1<sub>10</sub> – 1<sub>11</sub> transition near 14.9 GHz were detected with the 43 m NRAO telecope in several other dense dark clouds by\\ | Two hfs components of the 1<sub>10</sub> – 1<sub>11</sub> transition near 14.9 GHz were detected with the 43 m NRAO telecope in several other dense dark clouds by\\ |
| J. G. Mangum and A. Wooten,\\ | J. G. Mangum and A. Wooten,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1990A%26A...239..319M|Observations of the Cyclic C<sub>3</sub>H Radical in the Interstellar Medium]]**,\\ | **[[https://ui.adsabs.harvard.edu/abs/1990A%26A...239..319M|Observations of the Cyclic C<sub>3</sub>H Radical in the Interstellar Medium]]**,\\ |
| //Astron. Astrophys.// **239**, 319–325 (1990). | //Astron. Astrophys.// **239**, 319–325 (1990). |
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| The radical was also observed in three translucent molecular clouds CB 17, CB 24, and CB 228 by\\ | The radical was also observed in three translucent molecular clouds CB 17, CB 24, and CB 228 by\\ |
| B. E. Turner, E. Herbst, and R. Terzieva,\\ | B. E. Turner, E. Herbst, and R. Terzieva,\\ |
| **[[http://dx.doi.org/10.1086/313301|The Physics and Chemistry of Small Translucent Molecular Clouds. XIII. The Basic Hydrocarbon Chemistry]]**,\\ | **[[https://doi.org/10.1086/313301|The Physics and Chemistry of Small Translucent Molecular Clouds. XIII. The Basic Hydrocarbon Chemistry]]**,\\ |
| //Astrophys. J. Suppl. Ser.// **126**, 427–460 (2000). | //Astrophys. J. Suppl. Ser.// **126**, 427–460 (2000). |
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| The presence of //c//-C<sub>3</sub>H in the circumstellar envelopes of carbon rich late type stars was also established. E.g. CW Leo by\\ | The presence of //c//-C<sub>3</sub>H in the circumstellar envelopes of carbon rich late type stars was also established. E.g. CW Leo by\\ |
| J.Cernicharo, M. Guélin, and C. Kahane,\\ | J.Cernicharo, M. Guélin, and C. Kahane,\\ |
| **[[http://dx.doi.org/10.1051/aas:2000147|A λ 2 mm Molecular Line Survey of the C-star Envelope IRC+10216]]**,\\ | **[[https://doi.org/10.1051/aas:2000147|A λ 2 mm Molecular Line Survey of the C-star Envelope IRC+10216]]**,\\ |
| //Astron. Astrophys. Suppl. Ser.// **142**, 181–215 (2000).\\ | //Astron. Astrophys. Suppl. Ser.// **142**, 181–215 (2000).\\ |
| and LL Peg by\\ | and LL Peg by\\ |
| Y. Zhang, S. Kwok, and J.-I. Nakashima,\\ | Y. Zhang, S. Kwok, and J.-I. Nakashima,\\ |
| **[[http://dx.doi.org/10.1088/0004-637X/700/2/1262|A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths]]**,\\ | **[[https://doi.org/10.1088/0004-637X/700/2/1262|A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths]]**,\\ |
| //Astrophys. J.// **700**, 1262–1281 (2009). | //Astrophys. J.// **700**, 1262–1281 (2009). |
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| H. S. Liszt, J. Pety, M. Gerin, and R. Lucas,\\ | H. S. Liszt, J. Pety, M. Gerin, and R. Lucas,\\ |
| detected with the IRAM 30 m telescope\\ | detected with the IRAM 30 m telescope\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201323320|HCO, //c//-C<sub>3</sub>H and CF<sup>+</sup>: three new molecules in diffuse, translucent and “spiral-arm” clouds]]**\\ | **[[https://doi.org/10.1051/0004-6361/201323320|HCO, //c//-C<sub>3</sub>H and CF<sup>+</sup>: three new molecules in diffuse, translucent and “spiral-arm” clouds]]**\\ |
| //Astron. Astrophys.// **564**, Art. No. A64 (2014). | //Astron. Astrophys.// **564**, Art. No. A64 (2014). |
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| Contributor(s): H. S. P. Müller; 09, 2011; 10, 2017 | Contributor(s): H. S. P. Müller; 09, 2011; 10, 2017 |
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