Classical H II regions in the Magellanic Clouds. 1: Physical properties

Details Classical H II regions in the Magellanic Clouds. 1: Physical properties Classical H II regions in the Magellanic Clouds. 1: Physical properties

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.1338w&link_type=abstract

The Astronomical Journal, vol. 107, no. 4, p. 1338-1362

Mathematics

Logic

25

Balmer Series, Data Reduction, Emission Spectra, Interstellar Extinction, Magellanic Clouds, Metallicity, Orion Nebula, Radio Spectra, Star Formation, Stellar Spectra, Big Bang Cosmology, Charge Coupled Devices, Electron Density Profiles, Luminosity, Quadratures, Spectrographs, Spectrophotometers, Thermal Radiation

Scientific paper

In the first in a series of papers I present a detailed examination of the basic physical properties of a sample of classical H II regions in the Magellanic Clouds. Narrow band H alpha imaging is used to show that such objects are representative of the most common H II regions in the Clouds and that they display a wide range of morphological characteristics. Spectroscopic data show that, as a result of the low metal content, classical H II regions in the Clouds are systematically hotter than their Galactic counterparts. The data also suggest the existence of a correlation between the excitation of an H II region and its emission measure. The spectra of one object, DEM 243, indicates the presence of a low velocity shock passing through this H II region. I also discuss the characteristics of the extinction towards these objects and speculate that it arises from dust local to the H II regions themselves.

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