The continuum spectra of dust complexes associated with W3 Main, M42, W49A, and W51A

Details The continuum spectra of dust complexes associated with W3 Main, M42, W49A, and W51A The continuum spectra of dust complexes associated with W3 Main, M42, W49A, and W51A

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...316..258g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 316, May 1, 1987, p. 258-264.

Astronomy and Astrophysics

Astronomy

39

Astronomical Spectroscopy, Continuous Spectra, Cosmic Dust, Interstellar Matter, Nebulae, Astronomical Maps, H Ii Regions, Infrared Astronomy, Millimeter Waves

Scientific paper

This paper presents observations of dust clouds at 230.1 GHz with a 12-m telescope. Comparison of these data, obtained by a mixer receiver with a spectral resolving power of 64, with maps made previously at 3 mm, permits the separation of the thermal emission of the dust from the free-free emission of the background H II regions. From the continuum spectra resulting from these thermal fluxes combined with observations at shorter wavelengths made by others, color temperatures, effective solid angles, and optical depths averaged over the source regions are derived. The solid angles imply considerable small-scale structure within these dust regions, which is observed by telescopes with high angular resolution. The long-wave frequency dependence beta of the opacity is 1.2 for OMC-1 and about 2.0 for the other source regions. From the calculated IR luminosities and the dust and gas masses, it is found that the ratios of IR luminosity to gas mass (in solar units) are a few hundred for the W3A, W49A, and W51A complexes but 1200 for OMC-1.

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