Ammonia observations of the molecular clouds near S68, S140, OMC2 and S106

Details Ammonia observations of the molecular clouds near S68, S140, OMC2 and S106 Ammonia observations of the molecular clouds near S68, S140, OMC2 and S106

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980mnras.193..115l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 193, Oct. 1980, p. 115-128.

Astronomy and Astrophysics

Astrophysics

43

Ammonia, Interstellar Gas, Molecular Clouds, Astrophysics, Density Distribution, Hydrogen Atoms, Molecular Excitation, Noise Spectra, Signal To Noise Ratios

Scientific paper

Observations of the J = 1, K = 1 and J = 2, K = 2 ammonia inversion doublets at 23.69 and 23.72 GHz in the interstellar molecular clouds near S 68, S 140, OMC 2 and S 106 are discussed. Maps of the ammonia emission in S 68, S 140 and OMC 2 are presented and compared with observations of other interstellar molecules, particularly carbon monoxide and formaldehyde. Ammonia optical depths and rotation temperatures are also derived from observations of the four clouds. The densities of hydrogen molecules determined from the ammonia observations are found to be from one to two orders of magnitude less than those derived from 2-mm formaldehyde observations, which may be attributed to absorption by a low-density intervening cloud or clumping in the source. In the case of clumping, which is considered more likely than a core-halo structure, the model predicts a highly inhomogeneous medium containing numerous clumps of molecular hydrogen of density about 10 to the 6th/cu cm and filling factor 0.4/parsec along the line of sight, immersed in a more tenuous gas of density 1,000-10,000/cu cm.

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