EDP Sciences
Free access
Volume 390, Number 2, August I 2002
Page(s) 649 - 665
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20020424

A&A 390, 649-665 (2002)
DOI: 10.1051/0004-6361:20020424

The physical structure of Magellanic Cloud $\ion{H}{ii}$ regions

I. Dataset
R. Vermeij1, F. Damour2, J. M. van der Hulst1 and J-.P. Baluteau2

1  Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
2  Laboratoire d'Astrophysique de Marseille, CNRS & Université de Provence, BP 8, 13376, Marseille Cedex 12, France

(Received 26 October 2001 / Accepted 19 March 2002)

We present infrared and optical spectroscopic data for 11 $\ion{H}{ii}$ regions and one Supernova Remnant in the Large and Small Magellanic Cloud. The infrared data have been obtained with the Short Wavelength Spectrometer and Long Wavelength Spectrometer on board the Infrared Space Observatory as part of a Guaranteed Time Program on $\ion{H}{ii}$ regions in Local Group Galaxies. Aim of this project is to give a new and improved analysis of the physical structure of the sample $\ion{H}{ii}$ regions by combining as much spectral data as possible. A detailed account is given here of the reduction process, and the quality and reliability of the presented fluxes are discussed.

Key words: ISM: lines and bands -- $\ion{H}{ii}$ regions -- Magellanic Clouds

Offprint request: R. Vermeij, ronald@astro.rug.nl

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