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| molecules:ism:hocs-plus [2024/04/17 12:13] – mueller | molecules:ism:hocs-plus [2024/09/25 10:41] (current) – mueller |
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| //Astrophys. J.// **965**, Art. No. 149 (2024).\\ | //Astrophys. J.// **965**, Art. No. 149 (2024).\\ |
| The cation was detected in the course of a molecular line survey of the Galactic Center molecular cloud G+0.693–0.027 employing the Yebes 40 m and IRAM 30 m radio telecopes. The transitions cover 34 to 161 GHz with //J"// = 2, 3, 6 − 13 and //K<sub>a</sub>// = 0. These //K<sub>a</sub>// = 0 are all considerably blended with //K<sub>a</sub>// = 0 lines of HNC<sup>34</sup>S because their //B + C// values are nearly identical. The contribution of HNC<sup>34</sup>S could be accounted for accurately through lines of HNCS, OCS, and OC<sup>34</sup>S and turned out to be less than that of HOCS<sup>+</sup>. Several lines are slightly or more severely blended in addition, but this is in most cases also well accounted. The cation is about a factor of 400 less abundant than OCS, about a factor of 7 less abundant than the isoelectronic HNCS, about a factor of 31 less abundant than the isovalent HOCO<sup>+</sup>, but at least more than a factor of 2 more abundant than the lower energy isomer HCSO<sup>+</sup>, which was not detected.\\ | The cation was detected in the course of a molecular line survey of the Galactic Center molecular cloud G+0.693–0.027 employing the Yebes 40 m and IRAM 30 m radio telecopes. The transitions cover 34 to 161 GHz with //J"// = 2, 3, 6 − 13 and //K<sub>a</sub>// = 0. These //K<sub>a</sub>// = 0 are all considerably blended with //K<sub>a</sub>// = 0 lines of HNC<sup>34</sup>S because their //B + C// values are nearly identical. The contribution of HNC<sup>34</sup>S could be accounted for accurately through lines of HNCS, OCS, and OC<sup>34</sup>S and turned out to be less than that of HOCS<sup>+</sup>. Several lines are slightly or more severely blended in addition, but this is in most cases also well accounted. The cation is about a factor of 400 less abundant than OCS, about a factor of 7 less abundant than the isoelectronic HNCS, about a factor of 31 less abundant than the isovalent HOCO<sup>+</sup>, but at least more than a factor of 2 more abundant than the lower energy isomer HCSO<sup>+</sup>, which was not detected.\\ |
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| | V. Lattanzi, M. Sanz-Novo, V. M. Rivilla, M. Araki, H. A. Bunn, J. Martín-Pintado, I. Jiménez-Serra, and P. Caselli\\ |
| | published more recently on\\ |
| | **[[https://doi.org/10.1051/0004-6361/202451518|Advancing Spectroscopic Understanding of HOCS<sup>+</sup>: Laboratory Investigations and Astronomical Implications]]**\\ |
| | //Astron. Astrophys.// **689**, Art. No. A260 (2024).\\ |
| | After detection of HOCS<sup>+</sup> //a//-type transitions with //K<sub>a</sub>// > 0, it was possible to identify //K<sub>a</sub>// = 1 transitions in the line survey described above. Most of the transitions were heavily blended, but some were sufficiently clear. |
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| Contributor(s): H. S. P. Müller; 04, 2024 | Contributor(s): H. S. P. Müller; 04, 2024; 09, 2024 |
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