Pumping the interstellar (6, 3) ammonia maser

Details Pumping the interstellar (6, 3) ammonia maser Pumping the interstellar (6, 3) ammonia maser

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378..445b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 445-454. Research supported by Australian Research G

Astronomy and Astrophysics

Astrophysics

6

Ammonia, Astronomical Spectroscopy, Emission Spectra, Infrared Spectra, Interstellar Masers, Nebulae, Energy Levels, Hydroxyl Emission, Quantum Numbers, Star Formation, Water

Scientific paper

A numerical model of the excitation of ammonia in dense interstellar clouds predicts strong maser emission in various inversion doublet lines when infrared pumping to the lowest vibrationally excited state is included. Specifically the (6, 3) transition mases, while the (5, 3) and (4, 3) transitions are in normal emission, as observed in W51. Model conditions are H2 density between 10 to the 8th and 10 to the 10th/cu cm, NH3 column density 10 to the 18th/sq cm, and infrared temperature greater than 200 K, comparable with conditions required for OH and H2O masing in regions of star of star formation. The intensity of the maser emission depends on the infrared field, suggesting that time variations may be due to fluctuations in an infrared source.

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