This article has an erratum: [https://doi.org/10.1051/0004-6361:20010986-1]
Volume 376, Number 3, September IV 2001
|Page(s)||1040 - 1053|
|Published online||15 September 2001|
Modeling far-infrared emission from the HII region S125
Department of Physics and Astronomy, Arizona State University, Tempe, AZ 85287-1504, USA
2 Space Science Department, Rutherford Appleton Lab, Chilton, Oxon OX11 0QX, UK
Corresponding author: P. A. Aannestad, email@example.com
Accepted: 5 July 2001
We present ISO-LWS 45-180 μm spectral observations at 17 positions in the HII region S125. We model, as one integrated region, the far-IR continuum emission as well as the observed emissions in the radio continuum and in the 21 cm line, comparing two different model density distributions and several silicate-carbon dust models. The dust in the HII region is found to be severely depleted, while the dust in the PDR region has a normal dust/gas ratio, but with a major fraction of the mass in the form of the very small dust grains. Silicate-carbon dust must have strongly enhanced far-IR emissivities to be consistent with the observed spectra. It is found that the ionizing star alone does not power the infrared luminosity, but that additional sources of far-IR radiation must be present in a ring-like region surrounding the HII region. In this region the star accounts for about 50% of the observed emission. For most positions, the additional emission peaks at a wavelength around 70 μm.
Key words: HII regions / ISM: individual objects: S125 / ISM: dust, extinction / infrared: ISM
© ESO, 2001
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