Fig. 2.
Spectra of cluster 23 (top) and cluster 18 (bottom) highlighting the WR features in their spectra. The spectrum of cluster 23 is scaled down with a factor 2.8 to fit in the same scale. Left panel: spectral region around the He II 4686 Å line. The broad emission component is the signature of the presence of WR stars, the other WR lines (N III and C III) are not detected. The narrow component of He II is originating in the diffuse gas. Additionally, all the nebular emission lines are marked. Right panel: spectral region around the red WR bump. This emission bump is originated by C IV, tracing WC stars. Cluster 23 only shows a faint bump, while cluster 18 shows a very strong feature.
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