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The Fermi Gamma-ray Burst Monitor reported the possible detection of thegamma-ray counterpart of a binary black hole merger event, GW150914. We showthat the gamma-ray emission is caused by a relativistic outflow with Lorentzfactor larger than 10. Subsequently, debris outflow pushes the ambient gas toform a shock, which is responsible for the afterglow synchrotron emission. Wefind that the 1.4 GHz radio flux peaks at $\sim10^5$ sec after the bursttrigger. If the ambient matter is dense enough with density larger than$\sim10^{-2}$ cm$^{-3}$, then the peak radio flux is $\sim0.1$ mJy, which isdetectable with radio telescopes such as the Very Large Array. The opticalafterglow peaks earlier than the radio, and if the ambient matter density islarger than $\sim0.1$ cm$^{-3}$, the optical flux is detectable with largetelescopes such as the Subaru Hyper Suprime-Cam. To reveal the currentlyunknown mechanisms of the outflow and its gamma-ray emission associated withthe binary black hole merger event, follow-up electromagnetic observations ofafterglows are important. Detection of the afterglow will localize the skyposition of the gravitational wave and the gamma-ray emissions, and it willsupport the physical association between them.

Electromagnetic Afterglows Associated with Gamma-Ray Emission Coincident with Binary Black Hole Merger Event GW150914