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The gravitational waves (GWs) from a binary black hole (BBH) with massesbetween 10^4 and 10^7 Msun can be detected with the Laser Interferometer SpaceAntenna (LISA) once their orbital frequency exceeds 10^-4 - 10^-5 Hz. Thebinary separation at this stage is approximately a=100 R_g (gravitationalradius), and the orbital speed is of order v/c=0.1. We argue that at thisstage, the binary will be producing bright electromagnetic (EM) radiation viagas bound to the individual BHs. Both BHs will have their own photospheres inX-ray and possibly also in optical bands. Relativistic Doppler modulations andlensing effects will inevitably imprint periodic variability in the EMlight-curve, tracking the phase of the orbital motion, and serving as atemplate for the GW inspiral waveform. Advanced localization of the source byLISA weeks to months prior to merger will enable a measurement of this EM chirpby wide-field X-ray or optical instruments. A comparison of the phases of theGW and EM chirp signals will help break degeneracies between system parameters,and probe a fractional difference difference Delta v in the propagation speedof photons and gravitons as low as Delta v/c = O(10^-17).

The electromagnetic chirp of a compact binary black hole: a phase template for the gravitational wave inspiral