Fig. G.3.
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Predicted distribution of OB+WR binaries in the mass ratio, MWR/MOB, - logarithmic orbital period, log Porb, plane. The number in each pixel is coded in colour. The H-free and CHE WR stars are identified in 1D projection. The observed WR binaries (Foellmi et al. 2003; Foellmi 2004; Koenigsberger et al. 2014; Hainich et al. 2015; Shenar et al. 2016, 2018) are plotted with black.
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