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| molecules:ism:ch-plus [2021/07/14 10:37] – mueller | molecules:ism:ch-plus [2026/07/28 14:30] (current) – mueller |
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| //Astrophys. J.// **93**, 11–23 (1941);\\ | //Astrophys. J.// **93**, 11–23 (1941);\\ |
| He reportedly also observed the third line.\\ | He reportedly also observed the third line.\\ |
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| The detection of its pure rotational spectrum toward in the planetary nebula NGC 7027 was reported by\\ | The detection of its pure rotational spectrum toward in the planetary nebula NGC 7027 was reported by\\ |
| **[[https://doi.org/10.1086/310729|Discovery of Far-Infrared Pure Rotational Transitions of CH<sup>+</sup> in NGC 7027]]**\\ | **[[https://doi.org/10.1086/310729|Discovery of Far-Infrared Pure Rotational Transitions of CH<sup>+</sup> in NGC 7027]]**\\ |
| //Astrophys. J.// **483**, L65–L68 (1997).\\ | //Astrophys. J.// **483**, L65–L68 (1997).\\ |
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| More recently, interstellar methylidynium has been observed for the first time in high resolution and in absorption towards the star-forming region G10.6-0.4. Actually, as observation of the //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> is hampered by a terrestrial O<sub>2</sub> line, <sup>13</sup>CH<sup>+</sup> was observed instead:\\ | More recently, interstellar methylidynium has been observed for the first time in high resolution and in absorption towards the star-forming region G10.6-0.4. Actually, as observation of the //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> is hampered by a terrestrial O<sub>2</sub> line, <sup>13</sup>CH<sup>+</sup> was observed instead:\\ |
| //Astrophys. J.// **634**, L149–L152 (2005).\\ | //Astrophys. J.// **634**, L149–L152 (2005).\\ |
| Please note that the inferred rest-frequency is incorrect. Two alternative rest frequencies were proposed of which the higher one is quite appropriate.\\ | Please note that the inferred rest-frequency is incorrect. Two alternative rest frequencies were proposed of which the higher one is quite appropriate.\\ |
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| The //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> has been detected with the //Herschel// satellite in emission toward the Orion Bar by\\ | The //J// = 1 – 0 transition of <sup>12</sup>CH<sup>+</sup> has been detected with the //Herschel// satellite in emission toward the Orion Bar by\\ |
| //Astron. Astrophys.// **518**, Art. No. L118 (2010).\\ | //Astron. Astrophys.// **518**, Art. No. L118 (2010).\\ |
| These authors were the first to use the correct rest frequency of 835137.5 MHz.\\ | These authors were the first to use the correct rest frequency of 835137.5 MHz.\\ |
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| Higher-//J// transitions of CH<sup>+</sup> were also detected with the PACS instrument on board of the //Herschel// satellite in the disc around a Herbig Be star by:\\ | Higher-//J// transitions of CH<sup>+</sup> were also detected with the PACS instrument on board of the //Herschel// satellite in the disc around a Herbig Be star by:\\ |
| **[[https://doi.org/10.1051/0004-6361/201116678|Detection of CH<sup>+</sup> Emission from the Disc around HD 100546]]**\\ | **[[https://doi.org/10.1051/0004-6361/201116678|Detection of CH<sup>+</sup> Emission from the Disc around HD 100546]]**\\ |
| //Astron. Astrophys.// **530**, Art. No. L2 (2011).\\ | //Astron. Astrophys.// **530**, Art. No. L2 (2011).\\ |
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| D. A. Neufeld, M. Goto, T. R. Geballe, R. Güsten, K. M. Menten, and H. Wiesemeyer\\ | D. A. Neufeld, M. Goto, T. R. Geballe, R. Güsten, K. M. Menten, and H. Wiesemeyer\\ |
| //Astrophys. J.// **894**, Art. No. 37 (2020).\\ | //Astrophys. J.// **894**, Art. No. 37 (2020).\\ |
| They detected in addition the //v// = 1 − 0, //P//(6) to //R//(3) transitions of CH<sup>+</sup> around 3.5 μm using the iSHELL spectrograph at the Infrared Telescope Facility on Mauna Kea. The //P//(6) line, however, is severely blended with a hydrogen recombination line. A separate account is planned on this subject.\\ | They detected in addition the //v// = 1 − 0, //P//(6) to //R//(3) transitions of CH<sup>+</sup> around 3.5 μm using the iSHELL spectrograph at the Infrared Telescope Facility on Mauna Kea. The //P//(6) line, however, is severely blended with a hydrogen recombination line. A separate account is planned on this subject.\\ |
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| T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, A. Schwörer, and C. Comito\\ | T. Möller, P. Schilke, A. Schmiedeke, E. A. Bergin, D. C. Lis, Á. Sánchez-Monge, A. Schwörer, and C. Comito\\ |
| **[[https://doi.org/10.1051/0004-6361/202040203|//Herschel// observations of EXtraOrdinary Sources: Full //Herschel///HIFI Molecular Line Survey of Sagittarius B2(M)]]**\\ | **[[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).\\ | //Astron. Astrophys.// **651**, Art. No. A9 (2021).\\ |
| | They observed clearly the //J// = 2 − 1 transition of CD<sup>+</sup> near 906.8 GHz mostly in absorption. The //J// = 4 − 2 transition near 1811.2 GHz is seen weakly in absorption.\\ |
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| Contributor(s): H. S. P. Müller; 2003; 02, 2006; 03, 2007; 04, 2011; 05, 2020 | Contributor(s): H. S. P. Müller; 2003; 02, 2006; 03, 2007; 04, 2011; 05, 2020; 07, 2021. |
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