molecules:ism:sh-plus

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 The //N// = 1 – 0, //J// = 1 – 1, fine structure component of sulfaniumylidene or sulfanylium, SH<sup>+</sup>, near 683 GHz has recently been detected in absorption from ground with the APEX 12 m telescope toward the evolved massive star-forming region Sagittarius B2(M):\\ The //N// = 1 – 0, //J// = 1 – 1, fine structure component of sulfaniumylidene or sulfanylium, SH<sup>+</sup>, near 683 GHz has recently been detected in absorption from ground with the APEX 12 m telescope toward the evolved massive star-forming region Sagittarius B2(M):\\
 K. M. Menten, F. Wyrowski, A. Belloche, R. Güsten, L. Dedes, and H. S. P. Müller,\\ K. M. Menten, F. Wyrowski, A. Belloche, R. Güsten, L. Dedes, and H. S. P. Müller,\\
-**[[http://dx.doi.org/10.1051/0004-6361/201014363|Submillimeter Absorption from SH<sup>+</sup>, a New Widespread Interstellar Radical, <sup>13</sup>CH<sup>+</sup> and HCl]]**\\+**[[https://doi.org/10.1051/0004-6361/201014363|Submillimeter Absorption from SH<sup>+</sup>, a New Widespread Interstellar Radical, <sup>13</sup>CH<sup>+</sup> and HCl]]**\\
 //Astron. Astrophys.// **525**, (2011), Art. No. A77.\\ //Astron. Astrophys.// **525**, (2011), Art. No. A77.\\
-The absorption originates not only from the envelope of Sgr B2(M), but also from various spiral arm molecular clouds along the line of sight. The observation of the stronger //J// = 2 – 1 fine structure component of the same rotational transition near 526 GHz from ground is hampered by a strong terrestrial water line, but it can be observed from satellites such as //Herschel//. The weak 0 – 1 component near 329 GHz is affected by CO, //J// = 3 – 2 and by a line of <sup>34</sup>SO<sub>2</sub>.+The absorption originates not only from the envelope of Sgr B2(M), but also from various spiral arm molecular clouds along the line of sight. The observation of the stronger //J// = 2 – 1 fine structure component of the same rotational transition near 526 GHz from ground is hampered by a strong terrestrial water line, but it can be observed from satellites such as //Herschel//. The weak 0 – 1 component near 329 GHz is affected by CO, //J// = 3 – 2 and by a line of <sup>34</sup>SO<sub>2</sub>.\\
  
 Shortly thereafter, SH<sup>+</sup> was observed in emission in three fine structure components (two excited ones) with //Herschel//-HIFI toward W3 IRS5 in the course of a study by\\ Shortly thereafter, SH<sup>+</sup> was observed in emission in three fine structure components (two excited ones) with //Herschel//-HIFI toward W3 IRS5 in the course of a study by\\
 A. O. Benz, S. Bruderer, E. F. van Dishoeck, et al.,\\ A. O. Benz, S. Bruderer, E. F. van Dishoeck, et al.,\\
 on\\ on\\
-**[[http://dx.doi.org/10.1051/0004-6361/201014363|Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system]]**\\+**[[https://doi.org/10.1051/0004-6361/201014363|Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system]]**\\
 //Astron. Astrophys.// **521**, (2010), Art. No. L35.\\ //Astron. Astrophys.// **521**, (2010), Art. No. L35.\\
-Note that the article actually appeared before the one mentioned above.+Note that the article actually appeared before the one mentioned above.\\
  
 B. Godard, E. Falgarone, M. Gerin, D. C. Lis, M. De Luca, J. H. Black, J. R. Goicoechea, J. Cernicharo, D. A. Neufeld, K. M. Menten, and M. Emprechtinger,\\ B. Godard, E. Falgarone, M. Gerin, D. C. Lis, M. De Luca, J. H. Black, J. R. Goicoechea, J. Cernicharo, D. A. Neufeld, K. M. Menten, and M. Emprechtinger,\\
 reported on a\\ reported on a\\
-**[[http://dx.doi.org/10.1051/0004-6361/201117664|Comparative study of CH<sup>+</sup> and SH<sup>+</sup> absorption lines observed towards distant star-forming regions]]**\\+**[[https://doi.org/10.1051/0004-6361/201117664|Comparative study of CH<sup>+</sup> and SH<sup>+</sup> absorption lines observed towards distant star-forming regions]]**\\
 //Astron. Astrophys.// **540**, (2012), Art. No. A87.\\ //Astron. Astrophys.// **540**, (2012), Art. No. A87.\\
-The 525 GHz FS component of SH<sup>+</sup> was observed toward 8 continuum sources with the //Herschel///HIFI instrument.+The 525 GHz FS component of SH<sup>+</sup> was observed toward 8 continuum sources with the //Herschel///HIFI instrument.\\
  
 Z. Nagy, F. F. S. van der Tak, V. Ossenkopf, M. Gerin, F. Le Petit, J. Le Bourlot, J. H. Black, J. R. Goicoechea, C. Joblin, M. Röllig, and E. A. Bergin,\\ Z. Nagy, F. F. S. van der Tak, V. Ossenkopf, M. Gerin, F. Le Petit, J. Le Bourlot, J. H. Black, J. R. Goicoechea, C. Joblin, M. Röllig, and E. A. Bergin,\\
 studied\\ studied\\
-**[[http://dx.doi.org/10.1051/0004-6361/201220519|The chemistry of ions in the Orion Bar I. – CH<sup>+</sup>, SH<sup>+</sup>, and CF<sup>+</sup>\\+**[[https://doi.org/10.1051/0004-6361/201220519|The chemistry of ions in the Orion Bar I. – CH<sup>+</sup>, SH<sup>+</sup>, and CF<sup>+</sup>\\
 The effect of high electron density and vibrationally excited H<sub>2</sub> in a warm PDR surface]]**\\ The effect of high electron density and vibrationally excited H<sub>2</sub> in a warm PDR surface]]**\\
 //Astron. Astrophys.// **550**, (2013), Art. No. A96.\\ //Astron. Astrophys.// **550**, (2013), Art. No. A96.\\
-As for other hydrides, such as CH<sup>+</sup>, SH<sup>+</sup> was observed in emission.+As for other hydrides, such as CH<sup>+</sup>, SH<sup>+</sup> was observed in emission.\\
  
 +T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, A. Schwörer, and C. Comito\\
 +described\\
 +**[[https://doi.org/10.1051/0004-6361/202040203|//Herschel// observations of EXtraOrdinary Sources: Full //Herschel///HIFI Molecular Line Survey of Sagittarius B2(M)]]**\\
 +//Astron. Astrophys.// **651**, Art. No. A9 (2021).\\
 +They observed the //J// = 2 − 1 and 1 − 1 fine structure components of the //N// = 1 − 0 rotational transition of <sup>34</sup>SH<sup>+</sup> near 525.1 and 682.5 GHz, respectively, in absorption.\\
  
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-Contributor(s): H. S. P. Müller; 12, 2010; 07, 2014; 12, 2015.+----
  
 +Contributor(s): H. S. P. Müller; 12, 2010; 07, 2014; 12, 2015; 07, 2021.
  
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