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--- molecules:ism:mecn [2026/04/13 12:23] – mueller
+++ molecules:ism:mecn [2026/04/13 12:55] (current) – mueller
@@ Line 4: / Line 4: @@
 P. M. Solomon, K. B. Jefferts, A. A. Penzias, and R. W. Wilson,\\
 **[[https://ui.adsabs.harvard.edu/abs/1971ApJ...168L.107S|Detection of Millimeter Emission Lines from Interstellar Methyl Cyanide]]**\\
-//Astrophys. J.// **168**, L107–L110 (1971).
+//Astrophys. J.// **168**, L107–L110 (1971).\\
+\\
 The molecule was also detected toward dark clouds:\\
 H. E. Matthews and T. J. Sears,\\
 **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...267L..53M|Detection of the //J// = 1 – 0 transition of CH<sub>3</sub>CN]]**\\
-//Astrophys. J.// **267**, L53–L57 (1983).
+//Astrophys. J.// **267**, L53–L57 (1983).\\
+\\
 More recently, it was detected toward a low mass proto-star:\\
 S. Cazaux, A. G. G. M. Tielens, C. Ceccarelli, A. Castets, V. Wakelam, E. Caux, B. Parise, D. Teyssier,\\
 **[[https://doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\
-//Astrophys. J.// **593**, L51–L55 (2003).
+//Astrophys. J.// **593**, L51–L55 (2003).\\
+\\
 V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\
@@ Line 25: / Line 28: @@
 **[[https://doi.org/10.1051/0004-6361/201834467|Small-scale Physical and Chemical Structure of Diffuse and Translucent Molecular Clouds along the Line of Sight to Sgr B2]]**\\
 //Astron. Astrophys.// **623** Art. No. A68 (2019).\\
-Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds.
+Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds.\\
+\\
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@@ Line 36: / Line 40: @@
 E. C. Sutton, G. A. Blake, C. R. Masson, and T. G. Phillips,\\
 **[[https://ui.adsabs.harvard.edu/abs/1985ApJS...58..341S|Molecular Line Survey of Orion A from 215 to 247 GHz]]**\\
-//Astrophys. J. Suppl. Ser.// **58**, 341–378 (1985).
+//Astrophys. J. Suppl. Ser.// **58**, 341–378 (1985).\\
+\\
 CH<sub>2</sub>DCN was detected in several transitions at 2 and 1.3 mm with the IRAM 30 m telecope toward the IRc2 hot core of the Orion Molecular Cloud. The CH<sub>2</sub>DCN/CH<sub>3</sub>CN ratio is roughly 0.01, suggesting considerable molecular deuterium enrichment even in hot cores. Note that the H/D ratio is lower by a factor of three because of the three equivalent H atoms in the parent species.\\
 M. Gerin, F. Combes, G. Wlodarczak, T. Jacq, M. Guélin, P. Encrenaz, and C. Laurent,\\
 **[[https://ui.adsabs.harvard.edu/abs/1992A%26A...259L..35G|Interstellar Detection of Deuterated Methyl Cyanide]]**\\
-//Astron. Astrophys.// **259**, L35–L38 (1992).
+//Astron. Astrophys.// **259**, L35–L38 (1992).\\
+\\
 CH<sub>3</sub>C<sup>15</sup>N was detected first toward Sgr B2(N) in the course of a line survey around 1.3 mm with SEST by\\
 A. Nummelin, P. Bergman, Å. Hjalmarson, P. Friberg, W. M. Irvine, T. J. Millar, M. Ohishi, and S. Saito,\\
 **[[https://doi.org/10.1086/313126|A Three-Position Spectral Line Survey of Sagittarius B2 between 218 and 263 GHz. I. The Observational Data]]**\\
-//Astrophys. J. Suppl. Ser.// **117**, 427–529 (1998).
+//Astrophys. J. Suppl. Ser.// **117**, 427–529 (1998).\\
+\\
 A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\
@@ Line 52: / Line 59: @@
 **[[https://doi.org/10.1051/0004-6361/201527268|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]**\\
 //Astron. Astrophys.// **587**, Art. No. A91 (2016).\\
-They detected <sup>13</sup>CH<sub>3</sub><sup>13</sup>CN unumbiguously about a factor of 480 lower than the main species. They also observed CH<sub>2</sub>DCN with a ratio of about 0.004 with respect to CH<sub>3</sub>CN.
+They detected <sup>13</sup>CH<sub>3</sub><sup>13</sup>CN unumbiguously about a factor of 480 lower than the main species. They also observed CH<sub>2</sub>DCN with a ratio of about 0.004 with respect to CH<sub>3</sub>CN.\\
+\\
 H. Calcutt, J. K. Jørgensen, H. S. P. Müller, L. E. Kristensen, A. Coutens, T. L. Bourke, R. T. Garrod, M. V. Persson, M. H. D. van der Wiel, E. F. van Dishoeck, and S. F. Wampfler\\
@@ Line 58: / Line 66: @@
 **[[https://doi.org/10.1051/0004-6361/201732289|The ALMA-PILS survey: Complex nitriles towards IRAS 16293-2422]]**\\
 //Astron. Astrophys.// **616**, Art. No. A90 (2018).\\
-They detected CHD<sub>2</sub>CN toward source A and B with ratios to CH<sub>2</sub>DCN and CH<sub>3</sub>CN of about 1 to 23 to 360 and 1 to 29 to 200, respectively. The degree of deuteration is slightly higher in the doubly deuterated cyanomethane compared to the singly deuterated one, as is also found for other molecules.
+They detected CHD<sub>2</sub>CN toward source A and B with ratios to CH<sub>2</sub>DCN and CH<sub>3</sub>CN of about 1 to 23 to 360 and 1 to 29 to 200, respectively. The degree of deuteration is slightly higher in the doubly deuterated cyanomethane compared to the singly deuterated one, as is also found for other molecules.\\
+\\
@@ Line 66: / Line 75: @@
 P. F. Goldsmith, R. Krotkov, R. L. Snell, R. D. Brown, and P. Godfrey,\\
 **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...274..184G|Vibrationally excited CH<sub>3</sub>CN and HC<sub>3</sub>N in Orion]]**\\
-//Astrophys. J.// **274**, 184–194 (1983).
+//Astrophys. J.// **274**, 184–194 (1983).\\
+\\
 S. M. Fortman, J. P. McMillan, C. F. Neese, S. K. Randall, A. J. Remijan, T. L. Wilson, and F. C. De Lucia\\
 gave a brief account on the detection of //v//<sub>8</sub> = 2 in their work\\
 **[[https://doi.org/10.1016/j.jms.2012.08.002|An analysis of a preliminary ALMA Orion KL spectrum via the use of complete experimental spectra from the laboratory]]**\\
-//J. Mol. Spectrosc.// **280**, 11–20 (2012).
+//J. Mol. Spectrosc.// **280**, 11–20 (2012).\\
+\\
 A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\
@@ Line 84: / Line 95: @@
 **[[https://doi.org/10.1016/j.jms.2021.111449|Toward a Global Model of the Interactions in Low-lying States of Methyl Cyanide: Rotational and Rovibrational Spectroscopy of the v4 = 1 State and Tentative Interstellar Detection of the v4 = v8 = 1 State in Sgr B2(N)]]**\\
 //J. Mol. Spectrosc.// **378**, Art. No. 111449 (2021).\\
+In their survey Re-exploring Molecular Complexity with ALMA (ReMoCA) of Sagittarius B2(N) at 3 mm (84.1 - 114.4 GHz), CH<sub>3</sub>CN transitions up to //v//<sub>4</sub> = 1 were identified confidently in SgrB2(N1S), a position in the main hot core with relatively narrow lines. The global methyl cyanide model also indicates several lines in //v//<sub>4</sub> = //v//<sub>8</sub> = 1 to be well above the 3σ limit, but all but one lines are blended by much stronger lines.\\
+\\
+Some time later,\\
+H. S. P. Müller, A. Belloche, F. Lewen, and S. Schlemmer\\
+reported on\\
+**[[https://doi.org/10.1016/j.jms.2021.111449|Rotational Spectroscopy as a Tool to Study Vibration−Rotation Interaction: Investigations of (13)CH3CN and CH3(13)CN up to v8 = 2 and a Search for v8 = 2 Transitions toward Sagittarius B2(N)]]**\\
+//ACS Earth Space Chem.// **10**, 578 (2026).\\
+The same survey as in the previous paragraph aling with the extended model were used to try to identify v8 = 2 transitions of <sup>13</sup>CH<sub>3</sub>CN and of CH<sub>3</sub><sup>13</sup>CN. While according to the model some lines were expected to be above the 3σ limit, all these lines were blended with much stronger lines. Nevertheless, these observations indicate the need for these data.\\
+\\
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