Hot shocked ammonia towards SGR B2

Details Hot shocked ammonia towards SGR B2 Hot shocked ammonia towards SGR B2

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...294..815f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 294, no. 3, p. 815-824

Astronomy and Astrophysics

Astronomy

50

Ammonia, Interstellar Matter, Molecular Clouds, Shock Waves, Star Formation, H Ii Regions, Radio Astronomy, Sputtering, Stellar Temperature

Scientific paper

Metastable levels of ammonia up to (J, K) = (14, 14) have been observed in absorption towards SgrB2, a giant molecular cloud close to the galactic center. We investigate the physical conditions that can explain these and related observations and conclude that hot (500 K) and low density (103/cu cm) gas is responsible. We find that C-shock models are able to reproduce these conditions and hence the metastable column densities, providing that the formation of NH3 on grain surfaces and its sputtering by the shock wave are taken into account. The column density of NH2 predicted by the model of the hot ammonia regions is consistent with recent observations of SgrB2-M, but the H2O column density appears to be too high.

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