Molecular line survey of Sagittarius B2(M) from 330 to 355 GHz and comparison with Sagittarius B2(N)

Details Molecular line survey of Sagittarius B2(M) from 330 to 355 GHz and comparison with Sagittarius B2(N) Molecular line survey of Sagittarius B2(M) from 330 to 355 GHz and comparison with Sagittarius B2(N)

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apjs...77..255s&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 77, Oct. 1991, p. 255-285. Research supported by NASA, David and

Astronomy and Astrophysics

Astrophysics

80

H Ii Regions, Interstellar Masers, Interstellar Matter, Molecular Spectra, Water Masers, Astronomical Spectroscopy, Emission Spectra, Hydroxyl Emission, Interstellar Chemistry, Molecular Clouds, Sagittarius Constellation

Scientific paper

A submillimeter survey of Sgr B2 is described in which sufficient spatial resolution permitted the observation of some of the source structure. The position Sgr B2(M) is examined in relation to the submillimeter emission of Sgr B2(N) and previous millimeter observational data of source (M) at a lower spatial resolution. Because the submillimeter observations are more sensitive to core emission, the molecules SO2 and CH3OH tend to dominate the spectrum. The core emission is found to be similar to that of the Orion molecular cloud, and the submillimeter and millimeter lines have high optical depths. The (N) source has a much higher column density than that of (M) except for SO and SO2, and (N) also appears to have a higher excitation which can indicate a core with a higher density.

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