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I present a set of long-term, direct, relativistic many-body computations ofmodel dense stellar clusters with up-to-date stellar-evolutionary, supernova(SN), and remnant natal-kick models, including pair instability and pulsationpair instability supernova (PSN and PPSN), using an updated version of NBODY7N-body simulation program. The N-body model also includes stellarevolution-based natal spins of BHs and treatments of binary black hole (BBH)mergers based on numerical relativity. These, for the first time in a directN-body simulation, allow for second-generation BBH mergers. The set of 65evolutionary models have initial masses $10^4M_\odot-10^5M_\odot$, sizes 1 pc-3pc, metallicity $0.0001-0.02$, with the massive stars in primordial binariesand they represent young massive clusters (YMC) and moderately massive openclusters (OC). Such models produce dynamically-paired BBH mergers that agreewell with the observed masses, mass ratios, effective spin parameters, andfinal spins of the LVC O1/O2 merger events, provided BHs are born with low orno spin but spin up after undergoing a BBH merger or matter accretion onto it.In particular, the distinctly higher mass, effective spin parameter, and finalspin of GW170729 merger event is naturally reproduced, as also the massasymmetry of the O3 event GW190412. The computed models produce massive,$\sim100M_\odot$ BBH mergers with primary mass within the 'PSN gap' and alsoyield mergers involving remnants in the 'mass gap'. They also suggest that YMCsand OCs produce persistent, Local-Universe GW sources detectable by LISA. Suchclusters are also capable of producing eccentric LIGO-Virgo mergers.

monthly notices of the royal astronomical society

Stellar-mass black holes in young massive and open stellar clusters IV:  updated stellar-evolutionary and black hole spin models and comparisons with  the LIGO-Virgo O1/O2 merger-event data