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In the last few years before merger, supermassive black hole binaries willrapidly inspiral and precess in a magnetic field imposed by a surroundingcircumbinary disk. Multiple simulations suggest this relative motion willconvert some of the local energy to a Poynting-dominated outflow, with aluminosity 10^{43} erg/s * (B/10^4 G)^2(M/10^8 Msun)^2 (v/0.4 c)^2, some ofwhich may emerge as synchrotron emission at frequencies near 1 GHz wherecurrent and planned wide-field radio surveys will operate. On top of a secularincrease in power on the gravitational wave inspiral timescale, orbital motionwill produce significant, detectable modulations, both on orbital periods and(if black hole spins are not aligned with the binary's total angular momenta)spin-orbit precession timescales. Because the gravitational wave merger timeincreases rapidly with separation, we find vast numbers of these transients areubiquitously predicted, unless explicitly ruled out (by low efficiency$\epsilon$) or obscured (by accretion geometry f_{geo}). If the fraction ofPoynting flux converted to radio emission times the fraction of lines of sightaccessible $f_{geo}$ is sufficiently large (f_{geo} \epsilon > 2\times 10^{-4}for a 1 year orbital period), at least one event is accessible to future blindsurveys at a nominal 10^4 {deg}^2 with 0.5 mJy sensitivity. Our proceduregeneralizes to other flux-limited surveys designed to investigate EM signaturesassociated with many modulations produced by merging SMBH binaries.

Blindly detecting orbital modulations of jets from merging supermassive black holes