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The electromagnetic (EM) follow-up of a gravitational wave (GW) eventrequires to scan a wide sky region, defined by the so called "skymap", for thedetection and identification of a transient counterpart. We propose a novelmethod that exploits information encoded in the GW signal to construct a"detectability map", which represents the time-dependent ("when") probabilityto detect the transient at each position of the skymap ("where"). Focusing onthe case of a neutron star binary inspiral, we model the associated shortgamma-ray burst afterglow and macronova emission, using the probabilitydistributions of binary parameters (sky position, distance, orbit inclination,mass ratio) extracted from the GW signal as inputs. The resulting family ofpossible lightcurves is the basis to construct the detectability map. As apractical example, we apply the method to a simulated GW signal produced by aneutron star merger at 75 Mpc whose localization uncertainty is very large(about 1500 square degrees). We construct observing strategies based on thedetectability maps for optical, infrared and radio facilities, taking VST,VISTA and MeerKAT as prototypes. Assuming limiting fluxes of r ~ 24.5, J ~ 22.4(AB magnitudes) and 500 uJy @ 1.4 GHz for ~ 1000 s of exposure each, theafterglow and macronova emissions are successfully detected with a minimumobserving time of 7, 15 and 5 hours respectively.

Where and when: optimal scheduling of the electromagnetic follow-up of gravitational-wave events based on counterpart lightcurve models