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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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| More recently, it was detected toward a low mass proto-star:\\ | 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,\\ | S. Cazaux, A. G. G. M. Tielens, C. Ceccarelli, A. Castets, V. Wakelam, E. Caux, B. Parise, D. Teyssier,\\ |
| **[[http://dx.doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\ | **[[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). |
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| V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\ | V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\ |
| reported on\\ | reported on\\ |
| [[http://dx.doi.org/10.1051/0004-6361/201731495|Complex Organic Molecules in Diffuse Clouds along the Line of Sight to Sgr B2]]\\ | **[[https://doi.org/10.1051/0004-6361/201731495|Complex Organic Molecules in Diffuse Clouds along the Line of Sight to Sgr B2]]**\\ |
| //Astron. Astrophys.// **605** (2017), Art. No. L6.\\ | //Astron. Astrophys.// **605** (2017), Art. No. L6.\\ |
| The //J// = 5 – 4 and 6 – 5, //K// = 0 transitions of CH<sub>3</sub>CN were detected with ALMA near 92.0 and 110.4 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds and in one velocity component corresponding to diffuse clouds in the Scutum arm. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\ | The //J// = 5 – 4 and 6 – 5, //K// = 0 transitions of CH<sub>3</sub>CN were detected with ALMA near 92.0 and 110.4 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds and in one velocity component corresponding to diffuse clouds in the Scutum arm. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\ |
| V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\ | V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\ |
| continued their investigation of\\ | continued their investigation of\\ |
| [[http://dx.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]]\\ | **[[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).\\ | //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. |
| 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>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\\ | 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,\\ | A. Nummelin, P. Bergman, Å. Hjalmarson, P. Friberg, W. M. Irvine, T. J. Millar, M. Ohishi, and S. Saito,\\ |
| **[[http://dx.doi.org/10.1086/313126|A Three-Position Spectral Line Survey of Sagittarius B2 between 218 and 263 GHz. I. The Observational Data]]**\\ | **[[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). |
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| A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\ | A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\ |
| were\\ | were\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201527268|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]**\\ | **[[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).\\ | //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\\ | 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\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201732289|The ALMA-PILS survey: Complex nitriles towards IRAS 16293-2422]]**\\ | **[[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).\\ | //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. |
| 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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| A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\ | A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\ |
| investigated\\ | investigated\\ |
| **[[http://dx.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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