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| molecules:ism:hncnh [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:hncnh [2019/10/23 17:17] (current) – mueller |
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| B. A. McGuire, R. A. Loomis, C. M. Charness, J. F. Corby, G. A. Blake, J. M. Hollis, F. J. Lovas, P. R. Jewell, and A. J. Remijan,\\ | B. A. McGuire, R. A. Loomis, C. M. Charness, J. F. Corby, G. A. Blake, J. M. Hollis, F. J. Lovas, P. R. Jewell, and A. J. Remijan,\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/758/2/L33|Interstellar Carbodiimide (HNCNH): A New Astronomical Detection from the GBT PRIMOS Survey via Maser Emission Features]]**\\ | **[[https://doi.org/10.1088/2041-8205/758/2/L33|Interstellar Carbodiimide (HNCNH): A New Astronomical Detection from the GBT PRIMOS Survey via Maser Emission Features]]**\\ |
| //Astrophys. J.// **758**, Art. No. L33 (2012).\\ | //Astrophys. J.// **758**, Art. No. L33 (2012).\\ |
| The molecule displays tunneling splitting into two components separated by slightly less than 0.5 GHz. Four and a half pairs of transitions of the type //J//+1<sub>0,//J//+1</sub> ↔ //J//<sub>1,//J//</sub> with //J// between 15 and 19 would fall into the range of the 1–46 GHz line survey of Sagittarius B2(N), the frequencies of one pair (//J// = 16), however, fall into the 16–17 GHz gap. Both components were seen for //J// = 17 and 18, one for //J// = 19. The maser activity was explained by the energy level structure and the Einstein //A// values. No maser activity was expected and seen for the //J// = 15, and no maser activity is expected for //J// = 16. The authors also suggest that HNCNH is chemically enhanced with respect to the gas phase equilibrium with H<sub>2</sub>NCN either via evaporation from water ice or via non-LTE formation in the gas phase (possibly via dissociative recombination of cations such as H<sub>2</sub>NCNH<sup>+</sup>). | The molecule displays tunneling splitting into two components separated by slightly less than 0.5 GHz. Four and a half pairs of transitions of the type //J//+1<sub>0,//J//+1</sub> ↔ //J//<sub>1,//J//</sub> with //J// between 15 and 19 would fall into the range of the 1–46 GHz line survey of Sagittarius B2(N), the frequencies of one pair (//J// = 16), however, fall into the 16–17 GHz gap. Both components were seen for //J// = 17 and 18, one for //J// = 19. The maser activity was explained by the energy level structure and the Einstein //A// values. No maser activity was expected and seen for the //J// = 15, and no maser activity is expected for //J// = 16. The authors also suggest that HNCNH is chemically enhanced with respect to the gas phase equilibrium with H<sub>2</sub>NCN either via evaporation from water ice or via non-LTE formation in the gas phase (possibly via dissociative recombination of cations such as H<sub>2</sub>NCNH<sup>+</sup>). |
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| Contributor(s): H. S. P. Müller; 10, 2012 | Contributor(s): H. S. P. Müller; 10, 2012 |
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