Astronomy and Astrophysics – Astrophysics
Scientific paper
2000-03-22
Astrophys.J.539:641-657,2000
Astronomy and Astrophysics
Astrophysics
30 pages,incl. 11 figures, 3 tables; accepted for publication in the Astrophysical Journal. Postscript preprint also available
Scientific paper
10.1086/309261
We present new ISO-SWS data for a sample of 27 starburst galaxies, and with these data examine the issues of formation and evolution of the most massive stars in starburst galaxies. Using starburst models which incorporate time evolution, new stellar atmosphere models for massive stars, and a starburst model geometry derived from observations of the prototypical starburst M82, we model the integrated mid-infrared line ratio [NeIII](15.6 microns)/[NeII](12.8 microns). This line ratio is sensitive to the hardness of the stellar energy distribution and therefore to the most massive stars present. We conclude from our models, with consideration of recent determinations of the stellar census in local, high-mass star forming regions, that the [NeIII]/[NeII] ratios we measure are consistent with the formation of massive (~50-100 solar mass) stars in most starbursts. In this framework, the low nebular excitation inferred from the measured line ratios can be attributed to aging effects. By including estimates of the ratio of infrared-to-Lyman continuum luminosity for the galaxies in our sample, we further find that most starbursts are relatively short-lived (1-10 million years), only a few O-star lifetimes. We discuss a possible cause of such short events: the effectiveness of stellar winds and supernovae in destroying the starburst environment.
Forster-Schreiber Natascha M.
Genzel Reinhard
Kunze D.
Lutz Dieter
Spoon Henrik W. W.
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