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Recent observational results provide possible evidence that binary blackholes (BBHs) exist in the center of giant galaxies and may merge to form asupermassive black hole in the process of their evolution. We first detected aperiodic flux variation on a cycle of $93\pm1$ days from the 3-mm monitorobservations of a giant elliptical galaxy \object{3C 66B} for which an orbitalmotion with a period of $1.05\pm0.03$ years had been already observed. Thedetected signal period being shorter than the orbital period can be explainedby taking into consideration the Doppler-shifted modulation due to the orbitalmotion of a BBH. Assuming that the BBH has a circular orbit and that the jetaxis is parallel to the binary angular momentum, our observational resultsdemonstrate the presence of a very close BBH that has the binary orbit with anorbital period of $1.05\pm0.03$ years, an orbital radius of $(3.9\pm1.0) \times10^{-3}$ pc, an orbital separation of $(6.1^{+1.0}_{-0.9}) \times 10^{-3}$ pc,the larger black hole mass of $(1.2^{+0.5}_{-0.2}) \times 10^9$ $M_{\sun}$, andthe smaller black hole mass of $(7.0^{+4.7}_{-6.4}) \times 10^8$ $M_{\sun}$.The BBH decay time of $(5.1^{+60.5}_{-2.5})\times 10^2$ years provides evidencefor the occurrence of black hole mergers. This Letter will demonstrate theinteresting possibility of black hole collisions to form a supermassive blackhole in the process of evolution, one of the most spectacular natural phenomenain the universe.

A Very Close Binary Black Hole in a Giant Elliptical Galaxy 3C 66B and its Black Hole Merger