We investigate the future evolution of two extragalactic X-ray binaries : IC10 X-1 and NGC300 X-1 . Each of them consists of a high mass BH ( \sim 20 - 30 { ~ { } M } _ { \odot } ) accreting from a massive WR star companion ( \gtrsim 20 { ~ { } M } _ { \odot } ) , and both are located in low metallicity galaxies . We analyze the current state of the systems and demonstrate that both systems will very quickly ( \lesssim 0.3 Myr ) form close BH-BH binaries with the short coalescence time ( \sim 3 Gyr ) and large chirp mass ( \sim 15 { ~ { } M } _ { \odot } ) . The formation of BH-BH system seems unavoidable , as ( i ) WR companions are well within their Roche lobes and they do not expand so no Roche lobe overflow is expected , ( ii ) even intense WR wind mass loss does not remove sufficient mass to prohibit the formation of the second BH , ( ii ) even if BH receives the large natal kick , the systems are very closely bound and are almost impossible to disrupt . As there are two such immediate BH-BH progenitor systems within 2 Mpc and as the current gravitational wave instruments LIGO/VIRGO ( initial stage ) can detect such massive BH-BH mergers out to \sim 200 Mpc , the empirically estimated detection rate of such inspirals is R = 3.36 ^ { +8.29 } _ { -2.92 } at the 99 \% confidence level . If there is no detection in the current LIGO/VIRGO data ( unreleased year of s 6 run ) , the existence of these two massive BH systems poses an interesting challenge . Either the gravitational radiation search is not sensitive to massive inspirals or there is some fundamental misunderstanding of stellar evolution physics leading directly to the formation of BH-BH binaries .