molecules:ism:h2o-plus

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molecules:ism:h2o-plus [2019/02/25 22:38] – external edit 127.0.0.1molecules:ism:h2o-plus [2019/10/21 17:39] (current) – mueller
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 The //J// = 1.5 – 0.5 fine structure component of the 1<sub>11</sub> –0<sub>00</sub> transition of //ortho//-oxidaniumyl, //o//-H<sub>2</sub>O<sup>+</sup>, near 1115 GHz has recently been detected in absorption with the //Herschel// satellite toward the star-forming regions DR21, Sagittarius B2(M), and NGC 6334:\\ The //J// = 1.5 – 0.5 fine structure component of the 1<sub>11</sub> –0<sub>00</sub> transition of //ortho//-oxidaniumyl, //o//-H<sub>2</sub>O<sup>+</sup>, near 1115 GHz has recently been detected in absorption with the //Herschel// satellite toward the star-forming regions DR21, Sagittarius B2(M), and NGC 6334:\\
 V. Ossenkopf, H. S. P. Müller, D. C. Lis, et al.\\ V. Ossenkopf, H. S. P. Müller, D. C. Lis, et al.\\
-**[[http://dx.doi.org/10.1051/0004-6361/201014577|Detection of Interstellar Oxidaniumyl: Abundant H<sub>2</sub>O<sup>+</sup> towards the Star-forming Regions DR21, Sgr B2, and NGC6334]]**\\+**[[https://doi.org/10.1051/0004-6361/201014577|Detection of Interstellar Oxidaniumyl: Abundant H<sub>2</sub>O<sup>+</sup> towards the Star-forming Regions DR21, Sgr B2, and NGC6334]]**\\
 //Astron. Astrophys.// **518**, (2010) Art. No. L111.\\ //Astron. Astrophys.// **518**, (2010) Art. No. L111.\\
 While the spectra toward DR21 and NGC 6334 show partially resolved hyperfine structure, the spectrum toward Sgr B2(M) is rather complex because of additional absorption features caused by diffuse spiral arm clouds. While the spectra toward DR21 and NGC 6334 show partially resolved hyperfine structure, the spectrum toward Sgr B2(M) is rather complex because of additional absorption features caused by diffuse spiral arm clouds.
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 It is worthwhile mentioning that the same line was also observed in absorption toward several other sources. e.g. toward W31C (G10.6–0.4):\\ It is worthwhile mentioning that the same line was also observed in absorption toward several other sources. e.g. toward W31C (G10.6–0.4):\\
 M. Gerin, M. De Luca, J. Black, et al.\\ M. Gerin, M. De Luca, J. Black, et al.\\
-**[[http://dx.doi.org/10.1051/0004-6361/201014576|Interstellar OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup> and H<sub>3</sub>O<sup>+</sup> along the Sight-line to G10.6–0.4]]**\\+**[[https://doi.org/10.1051/0004-6361/201014576|Interstellar OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup> and H<sub>3</sub>O<sup>+</sup> along the Sight-line to G10.6–0.4]]**\\
 //Astron. Astrophys.// **518**, (2010) Art. No. L110.\\ //Astron. Astrophys.// **518**, (2010) Art. No. L110.\\
 This article presents also model calculation which indicate that in these sources OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> are formed in the mostly atomic diffuse ISM. This article presents also model calculation which indicate that in these sources OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> are formed in the mostly atomic diffuse ISM.
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 All four fine structure components of the 1<sub>10</sub> – 1<sub>01</sub> transition above 600 GHz have been detected in absorption with the //Herschel// satellite toward Sgr B2(M):\\ All four fine structure components of the 1<sub>10</sub> – 1<sub>01</sub> transition above 600 GHz have been detected in absorption with the //Herschel// satellite toward Sgr B2(M):\\
 P. Schilke, C. Comito, H. S. P. Müller, et al.,\\ P. Schilke, C. Comito, H. S. P. Müller, et al.,\\
-**[[http://dx.doi.org/10.1051/0004-6361/201015087|Herschel Observations of //ortho//- and //para//-Oxidaniumyl (H<sub>2</sub>O<sup>+</sup>) in Spiral Arm Clouds toward Sagittarius B2(M)]]**\\+**[[https://doi.org/10.1051/0004-6361/201015087|Herschel Observations of //ortho//- and //para//-Oxidaniumyl (H<sub>2</sub>O<sup>+</sup>) in Spiral Arm Clouds toward Sagittarius B2(M)]]**\\
 //Astron. Astrophys.// **521**, (2010) Art. No. L11.\\ //Astron. Astrophys.// **521**, (2010) Art. No. L11.\\
 The authors investigated the //ortho//-to-//para// ratio of the radical cation.\\ The authors investigated the //ortho//-to-//para// ratio of the radical cation.\\
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 P. Schilke, D. C. Lis, E. A. Bergin, R. Higgins, and C. Comito\\ P. Schilke, D. C. Lis, E. A. Bergin, R. Higgins, and C. Comito\\
 reported on the\\ reported on the\\
-**[[http://dx.doi.org/10.1021/jp312364c|//Ortho/////Para// Ratio of H<sub>2</sub>O<sup>+</sup> Toward Sagittarius B2(M) Revisited]]**\\+**[[https://doi.org/10.1021/jp312364c|//Ortho/////Para// Ratio of H<sub>2</sub>O<sup>+</sup> Toward Sagittarius B2(M) Revisited]]**\\
 //J. Phys. Chem. A// **117**, (2013) 9766.\\ //J. Phys. Chem. A// **117**, (2013) 9766.\\
 The derived values are now all compatible with the high temperature ratio of 3. The derived values are now all compatible with the high temperature ratio of 3.
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 Contributor(s): H. S. P. Müller; 07, 2010; 12, 2013 Contributor(s): H. S. P. Müller; 07, 2010; 12, 2013
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