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| molecules:ism:h2cnh [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:h2cnh [2019/10/23 17:10] (current) – mueller |
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| Methanimine, H<sub>2</sub>CNH, had been identified first in spectra recorded toward Sgr B2 by\\ | Methanimine, H<sub>2</sub>CNH, had been identified first in spectra recorded toward Sgr B2 by\\ |
| P. D. Godfrey, R. D. Brown, B. J. Robinson, and M. W. Sinclair,\\ | P. D. Godfrey, R. D. Brown, B. J. Robinson, and M. W. Sinclair,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1973ApL....13..119G|Discovery of Interstellar Methanimine (Formaldimine)]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1973ApL....13..119G|Discovery of Interstellar Methanimine (Formaldimine)]]**\\ |
| //Astrophys. Lett.// **13**, 119–121 (1973).\\ | //Astrophys. Lett.// **13**, 119–121 (1973).\\ |
| Even though only one transition, 1<sub>10</sub> –1<sub>11</sub> near 5290 MHz, was observed the detectionwas quite secure because of the <sup>14</sup>N hyperfine pattern. | Even though only one transition, 1<sub>10</sub> –1<sub>11</sub> near 5290 MHz, was observed the detectionwas quite secure because of the <sup>14</sup>N hyperfine pattern. |
| Methanimine turned out to be an abundant molecule not only in Sgr B2, but also in other hot core sources; e.g.:\\ | Methanimine turned out to be an abundant molecule not only in Sgr B2, but also in other hot core sources; e.g.:\\ |
| J. E. Dickens, W. M. Irvine, C. H. De Vries, and M. Ohishi,\\ | J. E. Dickens, W. M. Irvine, C. H. De Vries, and M. Ohishi,\\ |
| **[[http://dx.doi.org/10.1086/303884|Hydrogenation of Interstellar Molecules: A Survey for Methylenimine (CH<sub>2</sub>NH)]]**\\ | **[[https://doi.org/10.1086/303884|Hydrogenation of Interstellar Molecules: A Survey for Methylenimine (CH<sub>2</sub>NH)]]**\\ |
| //Astrophys. J.// **479**, 307–312 (1997).\\ | //Astrophys. J.// **479**, 307–312 (1997).\\ |
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| It was seen in absorption toward the dark cloud L183 and in emission in one of three translucent clouds (CB 17):\\ | It was seen in absorption toward the dark cloud L183 and in emission in one of three translucent clouds (CB 17):\\ |
| B. E. Turner, R. Terzieva, and E. Herbst,\\ | B. E. Turner, R. Terzieva, and E. Herbst,\\ |
| **[[http://dx.doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\ | **[[https://doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\ |
| //Astrophys. J.// **518**, 699–732 (1999). | //Astrophys. J.// **518**, 699–732 (1999). |
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| The detection of the <sup>13</sup>C isotopic species was reported in:\\ | The detection of the <sup>13</sup>C isotopic species was reported in:\\ |
| S.E. Cummins, R.A. Linke, and P. Thaddeus,\\ | S.E. Cummins, R.A. Linke, and P. Thaddeus,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1986ApJS...60..819C|A Survey of the Millimeter-Wave Spectrum of Sagittarius B2]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1986ApJS...60..819C|A Survey of the Millimeter-Wave Spectrum of Sagittarius B2]]**\\ |
| //Astrophys. J. Suppl. Ser.// **60**, 819–878 (1986). | //Astrophys. J. Suppl. Ser.// **60**, 819–878 (1986). |
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| Contributor(s): H. S. P. Müller; 06, 2006; 03, 2012 | Contributor(s): H. S. P. Müller; 06, 2006; 03, 2012 |
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