Anatomy of the Sagittarius complex. 3: Morphology and characteristics of the SGR B2 giant molecular giant molecular cloud

Details Anatomy of the Sagittarius complex. 3: Morphology and characteristics of the SGR B2 giant molecular giant molecular cloud Anatomy of the Sagittarius complex. 3: Morphology and characteristics of the SGR B2 giant molecular giant molecular cloud

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...280..208g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 280, no. 1, p. 208-220

Astronomy and Astrophysics

Astronomy

38

Continuous Spectra, Cosmic Dust, Far Infrared Radiation, H Ii Regions, Infrared Astronomy, Interstellar Matter, Molecular Clouds, Morphology, Radio Astronomy, Star Formation, Bolometers, Extremely High Frequencies, Infrared Astronomy Satellite, Millimeter Waves, Radio Telescopes, Submillimeter Waves

Scientific paper

This paper reports bolometric observations of dust emission from the giant star-forming H II/giant molecular cloud (GMC) complex Sgr B2, made at lambda 1300 micrometers and lambda 870 micrometer with the 30 m radio telescope of Institut de Radio Astronomie Millimetrique (IRAM) and at lambda 1300 micrometer and lambda 2.9 mm with the 15 m radio telescope of Swedish-ESO Submillimeter Telescope (SEST). Three compact (less than or equal to 0.4 pc) components of dust emission N(orth) = FIR1, M(iddle) = FIR2, and S(outh) = FIR3 are embedded within an extensive (4 pc x 11 pc) lower-density envelope. Combining the flux densities from our observations - corrected for free-free emission and molecular line emission - with others reported in the literature, we have produced continuum spectra for the integrated dust emission of the Sgr B2 complex and its 3 principal components. Based upon a spatial and spectral decomposition we determine the physical characteristics of the 4 components. We present and discuss new IRAS images of Sgr B2 and its surroundings. Sgr B2 appears in the lambda 100 micrometer and lambda 60 micrometer images as emission maxima where the lambda 100 micrometer/lambda 60 micrometer color temperature attains a value of about 35K. It appears that the dust inside this envelope of Sgr B2, seen at millimeter and submillimeter wavelengths, is too cold to be visible in the IRAS images that mainly trace the warmer diffuse dust and the dust in the outer skin of GMCs.

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