molecules:ism:ch-plus

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molecules:ism:ch-plus [2021/07/14 10:31] – muellermolecules: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.\\
 +\\
  
 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\\
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 **[[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).\\
 +\\
  
 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:\\
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 //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.\\
 +\\
  
 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\\
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 //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.\\
 +\\
  
 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:\\
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 **[[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).\\
 +\\
  
 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\\
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 //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.\\
 +\\
  
 +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 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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