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| **[[https://doi.org/10.1038/322524a0|An Interstellar Line Coincident with the P(2,1) Transition of Hydronium (H<sub>3</sub>O<sup>+</sup>)]]**\\ | **[[https://doi.org/10.1038/322524a0|An Interstellar Line Coincident with the P(2,1) Transition of Hydronium (H<sub>3</sub>O<sup>+</sup>)]]**\\ |
| //Nature// **322**, 524–626 (1986);\\ | //Nature// **322**, 524–626 (1986);\\ |
| with the NRAO 12 m telescope towards Orion KL; and\\ | with the NRAO 12 m telescope toward Orion KL; and\\ |
| A. Wootten, F. Boulanger, M. Bogey, F. Combes, P. J. Encrenaz, M. Gerin, and L. Ziurys,\\ | A. Wootten, F. Boulanger, M. Bogey, F. Combes, P. J. Encrenaz, M. Gerin, and L. Ziurys,\\ |
| **[[https://ui.adsabs.harvard.edu/abs/1986A%26A...166L..15W|A Search for Interstellar H<sub>3</sub>O<sup>+</sup>]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1986A%26A...166L..15W|A Search for Interstellar H<sub>3</sub>O<sup>+</sup>]]**\\ |
| //Astron. Astrophys.// **166**, L15–L18 (1986); with the NRAO 12 m telescope towards OMC-1 (essentially identical to Orion KL) and Sgr B2(OH).\\ | //Astron. Astrophys.// **166**, L15–L18 (1986); with the NRAO 12 m telescope toward OMC-1 (essentially identical to Orion KL) and Sgr B2(OH).\\ |
| **Note:** see below for the Orion KL case !\\ | **Note:** see below for the Orion KL case !\\ |
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| **[[https://doi.org/10.1086/186178|Detection of Interstellar H<sub>3</sub>O<sup>+</sup> – A Confirming Line]]**\\ | **[[https://doi.org/10.1086/186178|Detection of Interstellar H<sub>3</sub>O<sup>+</sup> – A Confirming Line]]**\\ |
| //Astrophys. J.// **380**, L79–L83 (1991),\\ | //Astrophys. J.// **380**, L79–L83 (1991),\\ |
| towards OMC-1, Sgr B2(OH) and (N). | toward OMC-1, Sgr B2(OH) and (N).\\ |
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| The 3<sub>0</sub><sup>+</sup> – 2<sub>0</sub><sup>–</sup> transition at 396272.412 MHz along with the previously mentioned transitions have been detected in several hot core sources:\\ | The 3<sub>0</sub><sup>+</sup> – 2<sub>0</sub><sup>–</sup> transition at 396272.412 MHz along with the previously mentioned transitions have been detected in several hot core sources:\\ |
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| | D. C. Lis, P. Schilke, E. A. Bergin, M. Emprechtinger, and the HEXOS Team\\ |
| | reported on\\ |
| | **[[https://doi.org/10.1098/rsta.2012.0025|Hot, Metastable Hydronium ion in the Galactic Centre: Formation Pumping in X-Ray-Irradiated Gas?]]**\\ |
| | //Phil. Trans. R. Soc. A// **370**, (2012) 5162.\\ |
| | Pure inversion transitions of H<sub>3</sub>O<sup>+</sup> with //J// = //K// up to 11 were detected with the HIFI instrument onboard the //Herschel// satellite toward Sagittarius B2(N). Two components were invoked to occur in the envelope of Sgr B2(N), one with a rotational temperature of about 160 K and one with about 520 K.\\ |
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| | Hot, metastable hydronium was also observed toward Sgr B2(M) and toward W31C outside the Galactic center by\\ |
| | D. C. Lis, P. Schilke, E. A. Bergin, M. Gerin, J. H. Black, C. Comito, M. De Luca, B. Godard, R. Higgins, F. Le Petit, J. C. Pearson, E. W. Pellegrini, T. G. Phillips, and S. Yu\\ |
| | **[[https://doi.org/10.1088/0004-637X/785/2/135|Widespread Rotationally Hot Hydronium Ion in the Galactic Interstellar Medium]]**\\ |
| | //Astrophys. J.// **785**, (2014) Art. No. 135.\\ |
| | Values of //T//<sub>rot</sub> were (re) determined as 177 ± 54 K and 546 ± 80 K for Sgr B2(M), 172 ± 51 K and 424 ± 48 K for Sgr B2(N), and about 62 K and 360 K for W31C; fewer transitions were detected for this last source and only up to //J// = //K// = 9.\\ |
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| Contributor(s): H. S. P. Müller; 01, 2008; 05, 2011 | Contributor(s): H. S. P. Müller; 01, 2008; 05, 2011; 02, 2026 |
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