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| molecules:ism:h3o-plus [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:h3o-plus [2019/10/22 17:07] (current) – mueller |
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| Two groups reported almost simultaneously the detection of the //J<sub>K</sub><sup>v<sub>t</sub></sup>// = 1<sub>1</sub><sup>–</sup> – 2<sub>1</sub><sup>+</sup> at 307192.41 MHz:\\ | Two groups reported almost simultaneously the detection of the //J<sub>K</sub><sup>v<sub>t</sub></sup>// = 1<sub>1</sub><sup>–</sup> – 2<sub>1</sub><sup>+</sup> at 307192.41 MHz:\\ |
| J. M. Hollis, E. B. Churchwell, E. Herbst, and F. C. de Lucia,\\ | J. M. Hollis, E. B. Churchwell, E. Herbst, and F. C. de Lucia,\\ |
| **[[http://dx.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 towards 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,\\ |
| **[[http://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 towards 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 ! |
| Later, additional transitions have been reported, e.g. the 3<sub>2</sub><sup>+</sup> – 2<sub>2</sub><sup>–</sup> transition at 364797.427 MHz:\\ | Later, additional transitions have been reported, e.g. the 3<sub>2</sub><sup>+</sup> – 2<sub>2</sub><sup>–</sup> transition at 364797.427 MHz:\\ |
| A. Wootten, J. G. Mangum, B. E. Turner, M. Bogey, F. Boulanger, F. Combes, P. J. Encrenaz, and M. Gerin,\\ | A. Wootten, J. G. Mangum, B. E. Turner, M. Bogey, F. Boulanger, F. Combes, P. J. Encrenaz, and M. Gerin,\\ |
| **[[http://dx.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). | towards OMC-1, Sgr B2(OH) and (N). |
| 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:\\ |
| T. G. Phlips, E. F. van Dishoek, J. Keene,\\ | T. G. Phlips, E. F. van Dishoek, J. Keene,\\ |
| **[[http://dx.doi.org/10.1086/171945|Interstellar H<sub>3</sub>O<sup>+</sup> and its Relation to the O<sub>2</sub> and H<sub>2</sub>O Abundances]]**\\ | **[[https://doi.org/10.1086/171945|Interstellar H<sub>3</sub>O<sup>+</sup> and its Relation to the O<sub>2</sub> and H<sub>2</sub>O Abundances]]**\\ |
| //Astrophys. J.// **399**, 533–550 (1992).\\ | //Astrophys. J.// **399**, 533–550 (1992).\\ |
| The sources, in which the cation reportedly was detected newly, are W3 IRS5 (aka W3 M), W3(OH), W51 M, and G34.3 +0.15. | The sources, in which the cation reportedly was detected newly, are W3 IRS5 (aka W3 M), W3(OH), W51 M, and G34.3 +0.15. |
| A line detected at 4.3121 (5) THz with KOA was tentativel assigned to the 4<sub>3</sub><sup>–</sup> – 3<sub>3</sub><sup>+</sup> transition:\\ | A line detected at 4.3121 (5) THz with KOA was tentativel assigned to the 4<sub>3</sub><sup>–</sup> – 3<sub>3</sub><sup>+</sup> transition:\\ |
| R. Timmermann, T. Nikola, A. Poglitsch, N. Geis, G. J. Stacey, and C. H. Townes,\\ | R. Timmermann, T. Nikola, A. Poglitsch, N. Geis, G. J. Stacey, and C. H. Townes,\\ |
| **[[http://dx.doi.org/10.1086/310055|Possible Discovery of the 70 Micron H<sub>3</sub>O<sup>+</sup> 4<sub>3</sub><sup>–</sup> – 3<sub>3</sub><sup>+</sup> Transition in Orion BN–IRc2]]**\\ | **[[https://doi.org/10.1086/310055|Possible Discovery of the 70 Micron H<sub>3</sub>O<sup>+</sup> 4<sub>3</sub><sup>–</sup> – 3<sub>3</sub><sup>+</sup> Transition in Orion BN–IRc2]]**\\ |
| //Astrophys. J.// **463**, L109–L112 (1996);\\ | //Astrophys. J.// **463**, L109–L112 (1996);\\ |
| three additional transitions were reported, one of which was overlapped with a line of H<sub>2</sub><sup>18</sup>O:\\ | three additional transitions were reported, one of which was overlapped with a line of H<sub>2</sub><sup>18</sup>O:\\ |
| J. R. Goicoechea and J. Cernicharo,\\ | J. R. Goicoechea and J. Cernicharo,\\ |
| **[[http://dx.doi.org/10.1086/321712|Far-Infrared Detection of H<sub>3</sub>O<sup>+</sup> in Sagittarius B2]]**,\\ | **[[https://doi.org/10.1086/321712|Far-Infrared Detection of H<sub>3</sub>O<sup>+</sup> in Sagittarius B2]]**,\\ |
| //Astrophys. J.// **554**, L213–L216 (2001). | //Astrophys. J.// **554**, L213–L216 (2001). |
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| Recent //Herschel///HIFI observations failed to detect any H<sub>3</sub>O<sup>+</sup> in Orion KL near 984.7, 1655.8, and 1657.25 GHz. Thus, previous reports on observations of this molecular ion in Orion KL could no be confirmed. It is possible that emission lines observed at lower frequencies (near 307.2, 364.8, and 396.3 GHz; see above) are caused by other species:\\ | Recent //Herschel///HIFI observations failed to detect any H<sub>3</sub>O<sup>+</sup> in Orion KL near 984.7, 1655.8, and 1657.25 GHz. Thus, previous reports on observations of this molecular ion in Orion KL could no be confirmed. It is possible that emission lines observed at lower frequencies (near 307.2, 364.8, and 396.3 GHz; see above) are caused by other species:\\ |
| H. Gupta, P. Rimmer, J. C. Pearson, et al.,\\ | H. Gupta, P. Rimmer, J. C. Pearson, et al.,\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201015117|Detection of OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> towards Orion KL]]**\\ | **[[https://doi.org/10.1051/0004-6361/201015117|Detection of OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> towards Orion KL]]**\\ |
| //Astron. Astrophys.// **521**, (2010) Art. No. L47. | //Astron. Astrophys.// **521**, (2010) Art. No. L47. |
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| Contributor(s): H. S. P. Müller; 01, 2008; 05, 2011 | Contributor(s): H. S. P. Müller; 01, 2008; 05, 2011 |
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