===== Reports on Carbodiimide, HNCNH, in the ISM =====

Carbodiimide, HNCNH, is a high energy isomer (1400 cm<sup>–1</sup> or 2000 K) of the fairly typical hot core molecule cyanamide, H<sub>2</sub>NCN. The molecule is thus very hard to detect under local thermodynamic equilibrium (LTE) conditions. Nevertheless,\\
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\\
**[[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).\\
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>).


----

Contributor(s): H. S. P. Müller; 10, 2012

----