Interpreting the H II Region Luminosity Function

Details Interpreting the H II Region Luminosity Function Interpreting the H II Region Luminosity Function

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mcdg.proc..185o&link_type=abstract

The Magellanic Clouds and Other Dwarf Galaxies, Proceedings of the Bonn/Bochum-Graduiertenkolleg Workshop, held at the Physikzen

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H Ii: Regions, Luminosity Function

Scientific paper

We construct Monte Carlo simulations of the H II region luminosity function (H II LF), drawing ionizing stars from a constant stellar IMF, and the number of ionizing stars from a power-law distribution of constant slope. We find that observed variations in the form of the H II LF across the Hubble sequence can be explained by a trend in the maximum number of ionizing stars per nebula. In addition, variations in the form of the H II LF between arm and interarm populations of spiral galaxies can be explained by evolutionary effects. The H II LF can thus reveal features in the most recent (< 10 Myr) star formation history of the host galaxies.

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