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If confirmed, a wide binary system of 70 $M_{\odot}$ black hole (BH) and an 8$M_{\odot}$ main sequence star (LB-1) is observed to reside in the Milky Way(MW). We show that long term evolution of an 8 $M_{\odot}$ star around a BHwith mass between 5-70 $M_{\odot}$ makes them visible as ultra-luminous X-ray(ULX) sources in the sky. Given the expected ULX phase lifetime ($\approx0.1$Myr) and their lack of detection in the MW, we conclude that the frequency ofan 8-20 $M_{\odot}$ star to be in binary around a stellar mass BH should beless than ($f<2\times10^{-3}$). This is in tension with Liu et al. (2019)claimed detection frequency of LB-1 like system around 8-20$M_{\odot}$ stars($f\approx3\times10^{-2}$). Moreover, the 8 $M_{\odot}$ star is likely to endas a neutron star (NS) born with a very small kick from an electron capturesupernova (ECSN), leaving behind a wide NS-BH binary. So far less than 1\% ofall the detectable pulsars in the MW are mapped and there has been no detectionof any pulsars in binary systems around BHs which sets an upper bound of about100 possible pulsar-BH systems in the MW. We show if the NS is born from ECSN,a frequency upper limit of ($f=5\times10^{-4}$) for stars with masses $\approx8-20~M_{\odot}$ in the MW to have a BH companion. The rate discrepancy willfurther increase as more pulsars are mapped in the MW, yet these searches wouldnot be able to rule out the Liu et al. detection frequency if NSs are insteadborn in core collapse SNe with the commonly inferred high kick velocities.

LB-1 is inconsistent with the X-ray source population and pulsar-black hole binary searches in the Milky Way