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| molecules:ism:hocs-plus [2024/04/17 10:53] – mueller | molecules:ism:hocs-plus [2024/09/25 10:41] (current) – mueller |
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| **[[https://doi.org/10.3847/1538-4357/ad2c01|Interstellar Detection of O-protonated Carbonyl Sulfide, HOCS<sup>+</sup>]]**\\ | **[[https://doi.org/10.3847/1538-4357/ad2c01|Interstellar Detection of O-protonated Carbonyl Sulfide, HOCS<sup>+</sup>]]**\\ |
| //Astrophys. J.// **965**, Art. No. 149 (2024).\\ | //Astrophys. J.// **965**, Art. No. 149 (2024).\\ |
| The cation was detected with the James Webb Space Telescope toward the protoplanetary disc d203-506 in the Orion Bar, which, in turn, is part of the Orion Nebula. The molecule was identified by its heavily mutually perturbed //v//<sub>2</sub> and //v//<sub>4</sub> bands near 1400 cm<sup>−1</sup> or ~7.2 //µ//m. The inferred rotational temperature is nearly 1000 K. Accurate laboratory data are not yet available for these two bands. The estimated spectroscopic parameters reproduce the spectrum reasonably well. Better parameters should be availbale soon.\\ | 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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