Other
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.6004k&link_type=abstract
American Astronomical Society, 182nd AAS Meeting, #60.04; Bulletin of the American Astronomical Society, Vol. 25, p.897
Other
Scientific paper
The infrared emission for a set of 70 hii regions, with known kinematic distances, was examined using images from the IRAS Sky Survey Atlas. These are radio bright (f_4860MHz > 1 Jy) hii regions located in the first Galactic quadrant: 30deg <~ l <~ 60deg , mid bmid <~ 0pdeg5 . The `typical' hii region in this sample has a dust temperature T(60/100) = 32K (for lambda (-2) emissivity law), a diameter of 30 pc, and a luminosity (lambda >= 50microns) of 10(5-10^6) L_&sun;. However, there are several noticeable exceptions which are associated with the molecular ring and the W43 and W51 hii region complexes. These hii regions are hotter than average and appear brighter than average at all IRAS wavebands. It is interesting to note that the hii regions associated with the W49 complex have characteristics typical of the sample. IRAS LRS data were available for 24 of the sample hii regions. The shapes of the spectra fell into two distinct classes based on the red (lambda >~ 12microns) end of the spectrum: flat or rising continua. Some of these spectra also showed silicate absorption at 10microns. All of these spectra are continuum dominated and show emission lines of [Nea II], [Nea III], or [Sa III]. Most of these lines are detected above the 3sigma threshold, however some of them are only at the 2sigma level. Also some of the spectra show an unidentified emission line at 21microns. The presence of the emission lines appear uncorrelated with any of the other IRAS properties. This suggests that the emission from the ionized gas may be spatially distinct from the dust emission.
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