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Among the four black hole binary merger events detected by LIGO, sixprogenitor black holes have masses greater than 20\,$M_\odot$. The existence ofsuch massive BHs calls for extreme metal-poor stars as the progenitors. Analternative possibility that a pair of stellar mass black holes each with mass$\sim7\,M_\odot$ increases to $>20\,M_\odot$ via accretion from a disksurrounding a super massive black hole in an active galactic nucleus isconsidered. The growth of mass of the binary and the transfer of orbitalangular momentum to the disk accelerates the merger. Based on the recentnumerical work of Tang et al. (2017), it is found that, in the disk of a lowmass AGN with mass $\sim10^6\,M_\odot$ and Eddington ratio $>0.01$, the mass ofan individual BH in the binary can grow to $>20\,M_\odot$ before coalescenceprovided that accretion takes place at a rate more than 10 times the Eddingtonvalue. The mechanism predicts a new class of gravitational wave sourcesinvolving the merger of two extreme Kerr black holes associated with activegalactic nuclei and a possible electromagnetic wave counterpart.

The growth of stellar mass black hole binaries trapped in an accretion disk of active galactic nuclei