Modeling of the continuum and molecular line emission from the Sagittarius B2 molecular cloud

Details Modeling of the continuum and molecular line emission from the Sagittarius B2 molecular cloud Modeling of the continuum and molecular line emission from the Sagittarius B2 molecular cloud

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..195l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 10, 1990, p. 195-210.

Astronomy and Astrophysics

Astrophysics

75

Emission Spectra, Molecular Clouds, Molecular Spectra, Abundance, Astronomical Models, Carbon Monoxide, Cosmic Dust, Interstellar Matter, Sagittarius Constellation, Temperature Distribution

Scientific paper

The continuum and molecular line emission from the Sagittarius B2 molecular cloud are modeled in order to determine the conditions in the core and the envelope of the cloud. The continuum models suggest that the total luminosity of the middle source Sgr B2(M) is an order of magnitude higher than that of the northern source Sgr B2(N). The microturbulent models of the molecular line emission predict the correct spatial intensity distribution of the J = 1 - 0 transitions of C(O-18) and (C-13)O. They have difficulties, however, reproducing the observed intensities of the higher transitions of these molecules. This may indicate that the envelope has a clumpy structure. Sgr B2 differs significantly from typical disk giant molecular clouds in that it has higher mass and luminosity of the continuum sources, much greater H2 column density and mean volume density, and different fractional abundances of many interstellar molecules.

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