The physical structure of Magellanic Cloud HII regions

Details The physical structure of Magellanic Cloud HII regions The physical structure of Magellanic Cloud HII regions

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..985v&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 985

Physics

Magellanic Clouds, Interstellar Medium, Elemental Abundances

Scientific paper

This paper presents some of the first results of a project aimed at determining in detail the physical conditions of star-forming regions. The project uses spectroscopic data obtained of 17 H II regions in the SMC and LMC. The data set consists of ISO-SWS, ISO-LWS and optical spectroscopic data covering a spectral range from 0.35 μm to 198 μm. The combination of optical and infrared data makes it possible to derive the detailed physical structure of an H II region. Quantities derived from this structure, e.g. improved chemical abundances and excitation source, will provide a link to the star-forming properties of these regions.

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