Populations of WC and WN stars in Wolf-Rayet galaxies

Details Populations of WC and WN stars in Wolf-Rayet galaxies Populations of WC and WN stars in Wolf-Rayet galaxies

1998-09-02

arxiv.org/abs/astro-ph/9809015v2

Astronomy and Astrophysics

Astrophysics

Accepted for publication in A&A. LaTeX using aa, psfigs and other macros. 19 pages including 13 figures. Paper and figures als

Scientific paper

We report the detection of WC stars in 5 Wolf-Rayet (WR) galaxies: He 2-10, NGC 3049, NGC 3125, NGC 5253 and Tol 89. The faint broad CIV5808 line requires sufficiently high S/N to be detected explaining the non-detection of this WC feature in previous observations. From the WR emission lines we conclude that all regions (except NGC 3049) contain a mixed population of WNL, and early WC stars. A spatial offset between the nebular emission and stellar light is observed in 2 objects. Due to age differences the nebular structures around the WR regions are possibly smaller than those mainly energized by SNe. The spatial distribution of WR stars follows the stellar continuum. We derive the absolute number of WR stars of different subtypes. The WC/WN ratios have typical values between 0.2-0.4, and show no clear trend with metallicity (Z). For low-Z objects, these values are larger than the observed WC/WN ratios in Local Group objects, but compatible with expectations for short bursts of if stellar evolution models with high mass loss are used. The ages of the starburst regions are 3-6 Myr; the burst duration must not exceed 2-4 Myr to account for the high population of WR stars, even if emission line stars similar to those in R136 and NGC 3603 are common in starbursts. Within the uncertainties most of the observed quantities are reproduced by models with a Salpeter IMF. Although some WR lines are stronger than predicted, no clear case requiring a significantly flatter IMF is found. IMF slopes much steeper than Salpeter may, however, not be compatible with our data. (Abridged abstract)

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