2024MNRAS.528.5119A

We present the first results of the DRAGON-II simulations, a suite of 19 N-body simulations of star clusters with up to 10⁶ stars, with up to 33 per cent of them initially paired in binaries. In this work, we describe the main evolution of the clusters and their compact objects (COs). All DRAGON-II clusters form in their centre a black hole (BH) subsystem with a density 10-100 times larger than the stellar density, with the cluster core containing $50{-}80~{{\rm per\ cent}}$ of the whole BH population. In all models, the BH average mass steeply decreases as a consequence of BH burning, reaching values 〈m_BH〉 < 15 M_⊙ within 10-30 relaxation times. Generally, our clusters retain only BHs lighter than 30 M_⊙ over 30 relaxation times. Looser clusters retain a higher binary fraction, because in such environments binaries are less likely disrupted by dynamical encounters. We find that BH-main-sequence star binaries have properties similar to recently observed systems. Double CO binaries (DCOBs) ejected from the cluster exhibit larger mass ratios and heavier primary masses than ejected binaries hosting single CO binaries (SCOBs). Ejected SCOBs have BH masses m_BH = 3-20 M_⊙, definitely lower than those in DCOBs (m_BH = 10-100 M_⊙).