The physical structure of magellanic cloud HII regions

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Abstract

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 HII 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 mu m to 198 mu m. The combination of optical and infrared data makes it possible to derive the detailed physical structure of an HII 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.

Original languageEnglish
Title of host publicationUNIVERSE AS SEEN BY ISO, VOLS I AND II
EditorsP Cox, MF Kessler
Place of PublicationPARIS
PublisherEUROPEAN SPACE AGENCY
Pages985-988
Number of pages4
ISBN (Print)92-9092-708-9
Publication statusPublished - 1999
EventConference on the Universe as Seen by ISO - , France
Duration: 20-Oct-199823-Oct-1998

Publication series

NameESA SPECIAL PUBLICATIONS
PublisherEUROPEAN SPACE AGENCY
Volume427
ISSN (Print)0379-6566

Other

OtherConference on the Universe as Seen by ISO
Country/TerritoryFrance
Period20/10/199823/10/1998

Keywords

  • Magellanic Clouds
  • interstellar medium
  • elemental abundances
  • WAVELENGTH SPECTROMETER

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