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--- molecules:ism:ch-plus [2020/05/12 13:49] – mueller
+++ molecules:ism:ch-plus [2021/07/14 10:58] (current) – mueller
@@ Line 13: / Line 13: @@
 **[[https://ui.adsabs.harvard.edu/abs/1941ApJ....93...11A|Some Results with the COUDÉ Spectrograph of the Mount Wilson Observatory]]**\\
 //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\\
 J. Cernicharo, X.-W. Liu, E. González-Alfonso, P. Cox, M. J. Barlow, T. Lim, and B. M. Swinyard,\\
 **[[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:\\
@@ Line 24: / Line 24: @@
 **[[https://doi.org/10.1086/499047|First Detection of <sup>13</sup>CH<sup>+</sup> (//J// = 1 – 0)]]**\\
 //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\\
@@ Line 38: / Line 38: @@
 **[[https://doi.org/10.1051/0004-6361/201014671|Strong CH<sup>+</sup> //J// = 1 – 0 Emission and Absorption in DR21]]**\\
 //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:\\
 W-F. Thi, F. Menard, G. Meeus, C. Martin-Zaidi, P. Woitke, E. Tatulli, M. Benisty, I. Kamp, I. Pascucci, C. Pinte, C. A. Grady, S. Brittain, G.J. White, C. D. Howard, G. Sandell, C. Eiroa,\\
 **[[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\\
@@ Line 49: / Line 49: @@
 **[[https://doi.org/10.3847/1538-4357/ab7191|Detection of Vibrational Emissions from the Helium Hydride Ion (HeH<sup>+</sup>) in the Planetary Nebula NGC 7027]]**\\
 //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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