Abstract Ultracompact dwarf galaxies (UCDs) are thought to be remnants of stripped galactic nuclei, among which a handful are known to host a central supermassive black hole (SMBH). As in stripped nuclear star clusters, the SMBHs in UCDs may be fed by stellar winds from old stellar populations, in the absence of substantial gas reservoirs and galactic inflows. In this work, we investigate such a wind-fed accretion scenario for M60-UCD1, which harbors a confirmed 2 × 10 7 M ⊙ SMBH and exhibits X-ray emission suggestive of SMBH accretion signature. Using three-dimensional hydrodynamical simulations, we simulate the SMBH accreting stellar winds from approximately 1500 asymptotic giant branch stars, and explore the role of ram pressure from the ambient interstellar or intracluster medium. After 5 Myr, the majority of the stellar winds form a cold gas disk (∼1000 M ⊙ ) within ∼10 pc as well as the SMBH’s gravitational sphere of influence. Within the inner 10 4 r g , this disk transitions into a hot (∼10 7 –10 9 K), geometrically thick corona that dominates the X-ray emission. The SMBH achieves an accretion rate of ∼10 −5 M ⊙ yr −1 , yielding an X-ray luminosity of ∼7 × 10 37 erg s −1 , consistent with observations. Including ram pressure stripping reduces both the accretion rate and luminosity by about a factor of 2. Our results suggest that the X-ray counterpart of M60-UCD1 originates from a weakly accreting SMBH fed by stellar winds, with broader insights into the feeding mechanisms of central massive black holes and the origins of X-ray sources in other UCDs.
Su et al. (2026) studied this question.