Representative thermal disk spectra before the coalescence (thin lines) and after (thick lines). The spectra are modified blackbody spectra of Eddington‐limited (﹩\dot{m}=1﹩) accretion disks around black holes of mass ﹩M=( 10^{4},\,10^{5},\,10^{6}) \,M_{\odot }﹩ (from right to left) and dimensionless spin parameter ﹩a_{*}=0.9﹩ (we ignored Doppler broadening). Only the emission from rings in the disk with ﹩r< 1000GM/ c^{2}﹩ was taken into account. These crude spectra are compatible with detailed models of Hubeny et al. (2001). We do not show thermal emission from any accretion disks around individual black holes that may be fed by the gas flow crossing the hollowed region.