Fig. 3.
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Mass distribution of compact objects in BH-NS mergers in the low-redshift Universe (z < 1) for models that employ a delayed supernova engine (M280, M283). There is no mass gap between NSs and BHs. It should be noted that our data become noisy for masses above ≳20 M⊙, although apparent decline in merger rate density for these higher masses is real and expected in our models.
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