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| molecules:ism:hc_no [2021/12/20 15:11] – mueller | molecules:ism:hc_no [2022/12/27 13:58] (current) – [Propynonyl, HCCCO] mueller |
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| See also HCCCO contribution.\\ | See also HCCCO contribution.\\ |
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| ==== HCCCO ==== | ==== Propynonyl, HCCCO ==== |
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| | J. Cernicharo, M. Agúndez, C. Cabezas, B. Tercero, N. Marcelino, R. Fuentetaja, J. R. Pardo, and P. de Vicente\\ |
| | reported on the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202142634|Discovery of HCCCO and C<sub>5</sub>O in TMC-1 with the QUIJOTE Line |
| | Survey]]**\\ |
| | //Astron. Astrophys.// **656**, Art. No. L21 (2021).\\ |
| | Propynonyl, HC<sub>3</sub>O, was identified through two rotational transitions with 2 ≤ //J// ≤ 4 in the course of a molecular line survey of the prototypical cold dark molecular cloud TMC-1 carried out with the Yebes 40 m radio telescope between 31.0 and 50.3 GHz. 7 of the 8 strong hyperfine components of four fine structure components were detected clearly; two HFS components were unresolved. A value of //T//<sub>rot</sub> = 7 K was taken from C<sub>3</sub>O. HC<sub>5</sub>O is the most abundant of the HC<sub>n</sub>O molecules with n ≥ 1. Setting its relative abundance to 100, they obtained for HCO, HC<sub>2</sub>O, HC<sub>3</sub>O, HC<sub>5</sub>O, and HC<sub>7</sub>O the approximate ratios 79 : 55 : 9 : 100 : 46. Only upper limits were derived for HC<sub>4</sub>O and HC<sub>6</sub>O; these were in both cases similar to those of HC<sub>3</sub>O and are thus somewhat constraining.\\ |
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| Contributor(s): H. S. P. Müller; 07, 2017; 12, 2017; 12, 2021 | Contributor(s): H. S. P. Müller; 07, 2017; 12, 2017; 12, 2021 |
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