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The question "what is the observable electromagnetic (EM) signature of acompact binary merger?" is an intriguing one with crucial consequences to thequest for gravitational waves (GW). Compact binary mergers are prime sources ofGW, targeted by current and next generation detectors. Numerical simulationshave demonstrated that these mergers eject energetic sub-relativistic (or evenrelativistic) outflows. This is certainly the case if the mergers produce shortGRBs, but even if not, significant outflows are expected. The interaction ofsuch outflows with the surround matter inevitably leads to a long lasting radiosignal. We calculate the expected signal from these outflows (our calculationsare also applicable to short GRB orphan afterglows) and we discuss theirdetectability. We show that the optimal search for such signal should,conveniently, take place around 1.4 GHz. Realistic estimates of the outflowparameters yield signals of a few hundred $\mu$Jy, lasting a few weeks, fromsources at the detection horizon of advanced GW detectors. Followup radioobservations, triggered by GW detection, could reveal the radio remnant evenunder unfavorable conditions. Upcoming all sky surveys can detect a few dozen,and possibly even thousands, merger remnants at any give time, therebyproviding robust merger rate estimates even before the advanced GW detectorsbecome operational. In fact, the radio transient RT 19870422 fits well theoverall properties predicted by our model and we suggest that its most probableorigin is a compact binary merger radio remnant.

Radio Remnants of Compact Binary Mergers - the Electromagnetic Signal that will follow the Gravitational Waves