Omega Centauri is dissolving. In ~15 Gyr, it will be gone. This workflow asks: what happens to the IMBH when its host cluster evaporates? Three stages trace the transition from stellar captive to naked wandering black hole in the Milky Way halo.
OC loses mass through both tidal stripping at each Galactic pericentre (~300 Myr orbital period) and continuous two-body evaporation. Current mass ~4 × 10⁶ M☉; dissolution (1% threshold) is expected in ~15–25 Gyr under nominal parameters.
During dissolution, the stellar cusp surrounding the IMBH depletes. The Brownian wander speed v_BH = σ × sqrt(⟨m★⟩/M_BH) drops as σ → 0. After full dissolution, the IMBH drifts through the Milky Way halo at the speed it had when the last stars departed — then wanders freely.
A naked wandering IMBH is detectable by several methods: Roman microlensing events (if it crosses dense fields), AXIS/Chandra X-ray emission from ISM Bondi accretion, and eventually LISA gravitational wave detection if it encounters a compact object. The detectability depends critically on the IMBH's location in the halo and the ISM density.
Computing…