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| molecules:ism:hcxn-plus [2024/06/26 18:02] – created mueller | molecules:ism:hcxn-plus [2024/07/31 16:17] (current) – mueller |
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| ===== On HC<sub>x</sub>N<sup>+</sup> in the ISM ===== | ===== On HCxN+ in the ISM ===== |
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| J. Cernicharo, B. Tercero, M. Agúndez, C. Cabezas, R. Fuentetaja, N. Marcelino and P. de Vicente\\ | J. Cernicharo, C. Cabezas, M. Agúndez, Y. Endo, B. Tercero, N. Marcelino and P. de Vicente\\ |
| reported on\\ | reported on the\\ |
| **[[https://doi.org/10.1051/0004-6361/202449531|CN and CCH Derivatives of Ethylene and Ethane: Confirmation of the Detection of CH<sub>3</sub>CH<sub>2</sub>CCH in TMC-1]]**\\ | **[[https://doi.org/10.1051/0004-6361/202450801|QUIJOTE discovery of the cation radicals HC5N+ and HC7N+]]**\\ |
| //Astron. Astrophys.// **686**, Art. No. A139 (2024).\\ | //Astron. Astrophys.// **686**, Art. No. L15 (2024).\\ |
| 1-Butyne, aka ethylacetylene, was identified through 9 unblended or slightly blended //a//-type transitions with 3 ≤ //J// ≤ 5 and //K<sub>a</sub>// ≤ 2 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 33.6 and 44.3 GHz. A value of //T//<sub>rot</sub> ≈ 9 K was derived. The column density of 1-butnyne is about a factor of 15 lower than that of butenyne.\\ | HC<sub>5</sub>N<sup>+</sup> and HC<sub>7</sub>N<sup>+</sup> were identified through 7 and 8 unblended or slightly blended transitions in their <sup>2</sup>Π<sub>3/2</sub> lower spin ladder, respectively, with 23/2 ≤ //J// ≤ 37/2 in the first case and 53/2 ≤ //J// ≤ 69/2 in the latter. The identifications were made 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. //T//<sub>rot</sub> = 8.5 ± 0.5 K was derived for HC<sub>5</sub>N<sup>+</sup>, while //T//<sub>rot</sub> = 7.8 ± 0.1 K was derived for HC<sub>7</sub>N<sup>+</sup>. The abundance ratios present a consistent and interesting picture. The HC<sub>5</sub>N<sup>+</sup> / HC<sub>7</sub>N<sup>+</sup> ratio is ~4.2; the HC<sub>5</sub>N<sup>+</sup> / HC<sub>5</sub>N, HC<sub>5</sub>N<sup>+</sup> / C<sub>5</sub>N<sup>−</sup>, and HC<sub>5</sub>N<sup>+</sup> / C<sub>5</sub>N<sup>−</sup> ratios are about 670, 4.8, and 1.2, respectively, while the HC<sub>7</sub>N<sup>+</sup> / HC<sub>7</sub>N and HC<sub>7</sub>N<sup>+</sup> / C<sub>7</sub>N<sup>−</sup> ratios are about 1000 and 2.2, respectively.\\ |
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| | Shortly thereafter,\\ |
| | C. Cabezas, M. Agúndez, Y. Endo, B. Tercero, N. Marcelino, P. de Vicente, and J. Cernicharo\\ |
| | published on the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202451081|Discovery of the interstellar cyanoacetylene radical cation HC3N+]]**\\ |
| | //Astron. Astrophys.// **687**, Art. No. L22 (2024).\\ |
| | The QUIJOTE survey of TMC-1 was employed once more to identify the six strong hyperfine structure components of the //J// = 7/2 − 5/2 near 31.63 GHz and 9/2 − 7/2 near 40.66 GHz in its <sup>2</sup>Π<sub>3/2</sub> lower spin ladder with good signal-to-noise ratio. The HFS components where not or only slightly blended with the exception of one in the upper transition. Supporting, but less favorable results were presented for the 11/2 − 9/2 transition near 49.965 GHz. The rotational temperature was estimated to be 4.5 K. The HC<sub>3</sub>N to HC<sub>3</sub>N<sup>+</sup> ratio is about 3200; the C<sub>3</sub>N to HC<sub>3</sub>N<sup>+</sup> ratio about 300; the HC<sub>3</sub>N<sup>+</sup> to HC<sub>5</sub>N<sup>+</sup> ratio is about 0.6.\\ |
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| Contributor(s): H. S. P. Müller; 06, 2024 | Contributor(s): H. S. P. Müller; 06, 2024; 07, 2024 |
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