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Fig. B.1. As Fig. 2, but for initial primary masses of 15.85 M ⊙ (top left), 17, 17 M ⊙ (top right), 19.19 M ⊙ (bottom left), and 39.81 M ⊙ (bottom right). The colour-coding indicates fates as in Fig. 2 (purple: L2-overflow, yellow: inverse mass transfer, green: mass-loss limit violation, and red: common-envelope evolution; all assumed to lead to a merger). Black hatching marks contact evolution, and the dark blue systems evolve to the OB+BH stage. Here, light blue marks systems where the mass donor is assumed to form a NS rather than a BH. The white line separates Case A and Case B evolution, and the area framed by the black line in the lower right corner marks the part of the parameter space that is disregarded in our results (see Sect. 2).

Fig. B.1. As Fig. 2, but for initial primary masses of 15.85 M ⊙ (top left), 17, 17 M ⊙ (top right), 19.19 M ⊙ (bottom left), and 39.81 M ⊙ (bottom right). The colour-coding indicates fates as in Fig. 2 (purple: L2-overflow, yellow: inverse mass transfer, green: mass-loss limit violation, and red: common-envelope evolution; all assumed to lead to a merger). Black hatching marks contact evolution, and the dark blue systems evolve to the OB+BH stage. Here, light blue marks systems where the mass donor is assumed to form a NS rather than a BH. The white line separates Case A and Case B evolution, and the area framed by the black line in the lower right corner marks the part of the parameter space that is disregarded in our results (see Sect. 2).

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Context. The recent gravitational wave measurements have demonstrated the existence of stellar mass black hole binaries. It is essential for our understanding of massive star evolution to identify the contribution of binary evolution to the formation of double black holes. Aims. A promising way to progress is investigating the progenitors of double...

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