  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)
