Panel a: series of equilibria of BH populations with individual BH mass, m_b = 10 M_⊙, expressed by the number of BHs, N_b, with respect to the BH population central density, ρ_b(0). The BH population is immersed in a Plummer profile of a globular cluster with average individual stellar mass, m_⋆ = 0.5 M_⊙, number of stars, N_⋆ = 10⁶, and half-mass radius, r_hm = 1 pc. For a BH subcluster with S >  0.185, corresponding here to N_b >  100, many equilibrium solutions exist. We consider S = 0.2, that is, N_b = 109 and the first three corresponding equilibria A, B, C. Panel b: density profile of the three stationary states A, B, C specified in panel a. Profile A is stable. The equilibria B and C are unstable with respect to Brownian fluctuations, although they may get stabilized by other processes.