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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\\ |
| E. C. Sutton, G. A. Blake, C. R. Masson, and T. G. Phillips,\\ | E. C. Sutton, G. A. Blake, C. R. Masson, and T. G. Phillips,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1985ApJS...58..341S|Molecular Line Survey of Orion A from 215 to 247 GHz]]**\\ | **[[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). |
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| 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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| S. M. Fortman, J. P. McMillan, C. F.Neese, S. K. Randall, A. J. Remijan, T. L. Wilson, and F. C. De Lucia\\ | 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\\ | 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]]**\\ | **[[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]]**\\ |
| **[[https://doi.org/10.1051/0004-6361/201321096|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]**\\ | **[[https://doi.org/10.1051/0004-6361/201321096|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]**\\ |
| //Astron. Astrophys.// **559**, Art. No. A47 (2013).\\ | //Astron. Astrophys.// **559**, Art. No. A47 (2013).\\ |
| Besides observing these two lower lying vibrational states, they detected transitions pertaining to //v//<sub>4</sub> = 1, the next higher state, as well as transitions of the <sup>13</sup>C isotopologs in their //v//<sub>8</sub> = 1 vibrational states. | Besides observing these two lower lying vibrational states, they detected transitions pertaining to //v//<sub>4</sub> = 1, the next higher state, as well as transitions of the <sup>13</sup>C isotopologs in their //v//<sub>8</sub> = 1 vibrational states.\\ |
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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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