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| molecules:ism:ch3c4h [2022/03/08 16:47] – mueller | molecules:ism:ch3c4h [2025/11/28 13:27] (current) – mueller |
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| **[[https://ui.adsabs.harvard.edu/abs/1984A%26A...134L..11W|Detection of interstellar methyldiacetylene (CH<sub>3</sub>C<sub>4</sub>H) in the dark dust cloud TMC 1]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1984A%26A...134L..11W|Detection of interstellar methyldiacetylene (CH<sub>3</sub>C<sub>4</sub>H) in the dark dust cloud TMC 1]]**\\ |
| //Astron. Astrophys.// **184**, L11–L14 (1984).\\ | //Astron. Astrophys.// **184**, L11–L14 (1984).\\ |
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| The molecule was also detected by\\ | The molecule was also detected by\\ |
| //Astrophys. J.// **847** Art. No. 51 (2017).\\ | //Astrophys. J.// **847** Art. No. 51 (2017).\\ |
| The three //J// = 11 – 10 transitions with //K// = 0, 1, and 2 were detected near 44.8 GHz with the 100 m GBT.\\ | The three //J// = 11 – 10 transitions with //K// = 0, 1, and 2 were detected near 44.8 GHz with the 100 m GBT.\\ |
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| C. Cabezas, R. Fuentetaja, E. Roueff, M. Agúndez, B. Tercero, N. Marcelino, J. R. Pardo, P. de Vicente and J. Cernicharo\\ | C. Cabezas, R. Fuentetaja, E. Roueff, M. Agúndez, B. Tercero, N. Marcelino, J. R. Pardo, P. de Vicente and J. Cernicharo\\ |
| //Astron. Astrophys.// **657** Art. No. L5 (2022).\\ | //Astron. Astrophys.// **657** Art. No. L5 (2022).\\ |
| Twelve transition with //J// = 8 to 12 and //K<sub>a</sub>// ≤ 1 were detected with the Yebes 40 m radio telescope. The CH<sub>3</sub>C<sub>4</sub>H to CH<sub>2</sub>DC<sub>4</sub>H abundance ratio of 24 ± 2 is very similar to that of CH<sub>3</sub>C<sub>3</sub>N to CH<sub>2</sub>DC<sub>3</sub>N ratio of 22 ± 2.\\ | Twelve transition with //J// = 8 to 12 and //K<sub>a</sub>// ≤ 1 were detected with the Yebes 40 m radio telescope. The CH<sub>3</sub>C<sub>4</sub>H to CH<sub>2</sub>DC<sub>4</sub>H abundance ratio of 24 ± 2 is very similar to that of CH<sub>3</sub>C<sub>3</sub>N to CH<sub>2</sub>DC<sub>3</sub>N ratio of 22 ± 2.\\ |
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| | More recently,\\ |
| | C. Cabezas, M. Agúndez, E. Roueff, R. Fuentetaja, B. Tercero, N. Marcelino, P. de Vicente, and J. Cernicharo\\ |
| | announced the\\ |
| | **[[https://doi.org/10.1051/202557754|Detection of Six Isotopologues of CH<sub>3</sub>CCCCH in TMC-1 with the QUIJOTE Line Survey]]**,\\ |
| | //Astron. Astrophys.// **703** Art. No. L22 (2025).\\ |
| | With an increase of the signal-to-noise ratio in comparison to the previous item, the authors were able to identify transition with //J// = 8 to 12 and //K<sub>a</sub>// ≤ 1 of all five singly substituted <sup>13</sup>C isotopologs and of CH<sub>3</sub>C<sub>4</sub>D with reasonable to good S/N and mostly not or only slightly blended. The lowest //J// pair of CH<sub>3</sub>C<sub>4</sub>D transitions was not covered. The <sup>12</sup>C/<sup>13</sup>C ratio is 93 ± 11, while the H/D ratio in the case of CH<sub>3</sub>C<sub>4</sub>D is 54 ± 8.\\ |
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| Contributor(s): H. S. P. Müller; 7, 2004; 10, 2017; 03, 2022 | Contributor(s): H. S. P. Müller; 7, 2004; 10, 2017; 03, 2022; 11, 2025 |
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