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Fig. 18.


Initial – final mass relation of white dwarfs (WD, MIST model from Cummings et al. 2018, blue), neutron stars (NS, red) and black holes (BH, purple) (PARSEC/SEVN model with Z = 0.0002 from Spera et al. 2015). Factors of two changes in Z are barely visible in the red (purple) line and do not affect the blue line. The lower green band indicates incomplete mass segregation because some of the main-sequence stars are more massive than the white dwarfs. The middle green band indicates the gap where no BHs have (yet) been detected. The upper green bands highlight the gap where pair-instability supernovae fully explode the progenitor star without leaving a black hole. The black line shows equality as a reference.

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