2025ApJ...995L..76P

Among the over 200 gravitational wave detections reported so far, GW231123 is a remarkable event that not only holds the record for the most massive black hole merger but also exhibits extreme spins. Its origin is actively debated. Proposed scenarios include dynamical formation through hierarchical mergers, Population III stars, accretion in active galactic nucleus disks and also more exotic explanations including primordial black holes and cosmic strings, each facing different challenges. Recent work showed that the incoming black holes of GW231123 could form from massive, rapidly rotating collapsing helium stars. Here, we address the question how such stars can be formed in very close binary systems and explore chemically homogeneous evolution (CHE) involving progenitors with masses above the pair-instability mass gap. We compute a grid of detailed massive binary models with the stellar evolution code MESA to follow the early evolution of binary progenitors and show that (i) very massive (M_i > 140 M_⊙) CHE binaries at low metallicity (Z = 10^–5) naturally produce rapidly rotating progenitors with high masses and high spins matching the properties of the black holes in GW231123 and (ii) the maximum spin of the progenitors is bound by their critical rotation rate, producing a tight correlation between the dimensionless spin and mass, a ∝ M^–0.9, in models without any hydrogen left. We conclude that the CHE channel appears to be a viable and natural scenario to produce progenitors. We compare and discuss the differences with earlier studies and comment on the large uncertainties in the final fate and collapse.