Fig. 5: Comparing the properties of isolated and dynamical NS–BH binary mergers.
From: Dissecting the properties of neutron star–black hole mergers originating in dense star clusters
a Chirp mass distribution for dynamical NS–BH mergers. Different colors correspond to different configurations (either a binary neutron star–star and a single black hole, NSSTBH, or viceversa, BHSTNS), velocity dispersion (σ) and metallicity (Z). The vertical dotted lines set the range allowed for isolated mergers. We provide the percentage of models with a chirp mass \({\cal{M}}_{{\mathrm{chirp}}} = 4{\mathrm{M}}_ \odot\), indicated by the dashed line. b Mass distribution of dynamical NS–BH mergers. The distribution of BH masses (mBH) is shown for different configurations, metallicity, and velocity dispersion. Open steps identify dynamical mergers, whereas filled gray step represent isolated mergers as calculated in Giacobbo et al.18. Labels indicate the probability to obtain a NS–BH merger with BH mass mBH > 20 M☉ for different configurations.
