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Fig. 4


Progenitor properties of “late” core-collapse supernovae for our standard simulation with binary stars. The normalized histograms show the distribution of the initial total mass Mtot, the initial mass of the primary, M1, and secondary, M2, the initial mass ratio, qM2/M1, and the initial orbital period P of binary systems that produce at least one core collapse after the last single star has exploded at around 48Myr.

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