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| molecules:ism:mecn [2019/05/09 12:35] – mueller | molecules:ism:mecn [2019/10/23 21:59] (current) – mueller |
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| Methyl cyanide, CH<sub>3</sub>CN, also known as acetonitrile or cyanomethane, was among the molecules detected early by radioastronomical means. The //J// = 6 – 5 transitions with //K// = 0 to 5 were observed with the 36 foot NRAO antenna at 2.7 mm toward Sagittarius B; some lines were probably also detected toward Sgr A where the lines were much broader.\\ | Methyl cyanide, CH<sub>3</sub>CN, also known as acetonitrile or cyanomethane, was among the molecules detected early by radioastronomical means. The //J// = 6 – 5 transitions with //K// = 0 to 5 were observed with the 36 foot NRAO antenna at 2.7 mm toward Sagittarius B; some lines were probably also detected toward Sgr A where the lines were much broader.\\ |
| P. M. Solomon, K. B. Jefferts, A. A. Penzias, and R. W. Wilson,\\ | P. M. Solomon, K. B. Jefferts, A. A. Penzias, and R. W. Wilson,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1971ApJ...168L.107S|Detection of Millimeter Emission Lines from Interstellar Methyl Cyanide]]**\\ | **[[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). |
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| The molecule was also detected toward dark clouds:\\ | The molecule was also detected toward dark clouds:\\ |
| H. E. Matthews and T. J. Sears,\\ | H. E. Matthews and T. J. Sears,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1983ApJ...267L..53M|Detection of the //J// = 1 – 0 transition of CH<sub>3</sub>CN]]**\\ | **[[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). |
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| CH<sub>3</sub><sup>13</sup>CN was probably detected because its lines are very close to those of the main isotopolog:\\ | CH<sub>3</sub><sup>13</sup>CN was probably detected because its lines are very close to those of the main isotopolog:\\ |
| S. E. Cummins, S. Green, P. Thaddeus, and R. A. Linke,\\ | S. E. Cummins, S. Green, P. Thaddeus, and R. A. Linke,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1983ApJ...266..331C|The Kinetic Temperature and Density of the Sagittarius B2 Molecular Cloud from Observations of Methyl Cyanide]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...266..331C|The Kinetic Temperature and Density of the Sagittarius B2 Molecular Cloud from Observations of Methyl Cyanide]]**\\ |
| //Astrophys. J.// **266**, 331–338 (1983);\\ | //Astrophys. J.// **266**, 331–338 (1983);\\ |
| both <sup>13</sup>C species were detected by\\ | both <sup>13</sup>C species were detected by\\ |
| 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.\\ | 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,\\ | M. Gerin, F. Combes, G. Wlodarczak, T. Jacq, M. Guélin, P. Encrenaz, and C. Laurent,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1992A%26A...259L..35G|Interstellar Detection of Deuterated Methyl Cyanide]]**\\ | **[[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). |
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| CH<sub>3</sub>CN in its lowest //v//<sub>8</sub> = 1 excited vibrational state was detected with the FCRAO near 111 GHz by\\ | CH<sub>3</sub>CN in its lowest //v//<sub>8</sub> = 1 excited vibrational state was detected with the FCRAO near 111 GHz by\\ |
| P. F. Goldsmith, R. Krotkov, R. L. Snell, R. D. Brown, and P. Godfrey,\\ | P. F. Goldsmith, R. Krotkov, R. L. Snell, R. D. Brown, and P. Godfrey,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1983ApJ...274..184G|Vibrationally excited CH<sub>3</sub>CN and HC<sub>3</sub>N in Orion]]**\\ | **[[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). |
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| Contributor(s): H. S. P. Müller 01, 2010; 10, 2017; 08, 2018; 01, 2019 | Contributor(s): H. S. P. Müller 01, 2010; 10, 2017; 08, 2018; 01, 2019 |
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