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| The //N// = 1 – 0, //J// = 0 – 1, fine structure component of oxidaniumylidene or hydroxylium, OH<sup>+</sup>, near 909 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// = 0 – 1, fine structure component of oxidaniumylidene or hydroxylium, OH<sup>+</sup>, near 909 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):\\ |
| F. Wyrowski, K. M. Menten, R. Güsten, and A. Belloche\\ | F. Wyrowski, K. M. Menten, R. Güsten, and A. Belloche\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201014364|First Interstellar Detection of OH<sup>+</sup>]]**\\ | **[[https://doi.org/10.1051/0004-6361/201014364|First Interstellar Detection of OH<sup>+</sup>]]**\\ |
| //Astron. Astrophys.// **518**, (2010), Art. No. A26.\\ | //Astron. Astrophys.// **518**, (2010), Art. No. A26.\\ |
| Interestingly, this is the weakest of the three fine structure components. | Interestingly, this is the weakest of the three fine structure components. |
| More recently, the strongest fine structure component near 972 GHz has been detected with the //Herschel// satellite toward several other sources, in particular toward W31C (G10.6–0.4), also in absorption:\\ | More recently, the strongest fine structure component near 972 GHz has been detected with the //Herschel// satellite toward several other sources, in particular toward W31C (G10.6–0.4), also in absorption:\\ |
| 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.\\ |
| Model calculations were carried out indicating that OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> are formed in the mostly atomic diffuse ISM in these sources. | Model calculations were carried out indicating that OH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> are formed in the mostly atomic diffuse ISM in these sources. |
| F. F. S. van der Tak, Z. Nagy, V. Ossenkopf, Z. Makai, J. H. Black, A. Faure, M. Gerin, and E. A. Bergin\\ | F. F. S. van der Tak, Z. Nagy, V. Ossenkopf, Z. Makai, J. H. Black, A. Faure, M. Gerin, and E. A. Bergin\\ |
| report on\\ | report on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201322164|Spatially Extended OH<sup>+</sup> Emission from the Orion Bar and Ridge]]**\\ | **[[https://doi.org/10.1051/0004-6361/201322164|Spatially Extended OH<sup>+</sup> Emission from the Orion Bar and Ridge]]**\\ |
| //Astron. Astrophys.// **560**, (2013) Art. No. A95.\\ | //Astron. Astrophys.// **560**, (2013) Art. No. A95.\\ |
| OH<sup>+</sup> in emission was also detected toward the Crab Nebula supernova remnant, also known as M 1, by:\\ | OH<sup>+</sup> in emission was also detected toward the Crab Nebula supernova remnant, also known as M 1, by:\\ |
| M. J. Barlow, B. M. Swinyard, P. J. Owen, J. Cernicharo, H. L. Gomez, R. J. Ivison, O. Krause, T. L. Lim, M. Matsuura, S. Miller, G. Olofsson, and E. T. Polehampton,\\ | M. J. Barlow, B. M. Swinyard, P. J. Owen, J. Cernicharo, H. L. Gomez, R. J. Ivison, O. Krause, T. L. Lim, M. Matsuura, S. Miller, G. Olofsson, and E. T. Polehampton,\\ |
| **[[http://dx.doi.org/10.1126/science.1243582|Detection of a Noble Gas Molecular Ion, <sup>36</sup>ArH<sup>+</sup>, in the Crab Nebula]]**\\ | **[[https://doi.org/10.1126/science.1243582|Detection of a Noble Gas Molecular Ion, <sup>36</sup>ArH<sup>+</sup>, in the Crab Nebula]]**\\ |
| //Science// **342**, (2013) 1343.\\ | //Science// **342**, (2013) 1343.\\ |
| Both observations were made with the //Herschel// satellite. | Both observations were made with the //Herschel// satellite. |
| An unspecified electronic transition at 385.3769 nm or 27903.58 cm<sup>–1</sup> was detected in diffuse clouds toward several stars at ESO Paranal observatory by:\\ | An unspecified electronic transition at 385.3769 nm or 27903.58 cm<sup>–1</sup> was detected in diffuse clouds toward several stars at ESO Paranal observatory by:\\ |
| J. Krelowski, Y. Beletsky, and G. A. Galazutdinov,\\ | J. Krelowski, Y. Beletsky, and G. A. Galazutdinov,\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/719/1/L20|Hydroxyl Cation in Translucent Interstellar Clouds]]**\\ | **[[https://doi.org/10.1088/2041-8205/719/1/L20|Hydroxyl Cation in Translucent Interstellar Clouds]]**\\ |
| //Astrophys. J.// **719**, (2010) L20.\\ | //Astrophys. J.// **719**, (2010) L20.\\ |
| This is the //R//(0) origin transition of the //v// = 0 – 0 vibrational band belonging to the //A// – //X// electronic transition which had been investigated by:\\ | This is the //R//(0) origin transition of the //v// = 0 – 0 vibrational band belonging to the //A// – //X// electronic transition which had been investigated by:\\ |
| A. J. Merer, D. N. Malm, R. W. Martin, M. Horani, and J. Rostas,\\ | A. J. Merer, D. N. Malm, R. W. Martin, M. Horani, and J. Rostas,\\ |
| **[[http://rparticle.web-p.cisti.nrc.ca/rparticle/AbstractTemplateServlet?calyLang=eng&journal=cjp&volume=53&year=0&issue=3&msno=p75-037|The Ultraviolet Emission Spectra of OH<sup>+</sup> and OD<sup>+</sup>. Rotational Structure and Perturbations in the //A// <sup>3</sup>Π<sub>//i//</sub> – //X// <sup>3</sup>Σ<sup>–</sup> Transition]]**\\ | **[[https://doi.org/10.1139/p75-037|The Ultraviolet Emission Spectra of OH<sup>+</sup> and OD<sup>+</sup>. Rotational Structure and Perturbations in the //A// <sup>3</sup>Π<sub>//i//</sub> – //X// <sup>3</sup>Σ<sup>–</sup> Transition]]**\\ |
| //Can. J. Phys.// **53**, (2010) 251. | //Can. J. Phys.// **53**, (1975) 251. |
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| Contributor(s): H. S. P. Müller; 07 & 08, 2010; 12, 2013. | Contributor(s): H. S. P. Müller; 07 & 08, 2010; 12, 2013. |
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