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--- molecules:ism:h3o-plus [2019/10/22 17:07] – mueller
+++ molecules:ism:h3o-plus [2026/02/05 13:04] (current) – mueller
@@ Line 5: / Line 5: @@
 **[[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);\\
-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,\\
 **[[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 !\\
+\\
 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:\\
@@ Line 15: / Line 16: @@
 **[[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),\\
-towards OMC-1, Sgr B2(OH) and (N).
+toward 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:\\
@@ Line 21: / Line 23: @@
 **[[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).\\
-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:\\
@@ Line 30: / Line 33: @@
 J. R. Goicoechea and J. Cernicharo,\\
 **[[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).\\
+\\
 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.,\\
 **[[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.\\
+\\
+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.\\
+\\
+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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