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The first direct detection of gravitational waves (GW) by the ground-basedinterferometers is expected to occur within the next few years. Theseinterferometers will detect the mergers of compact object binaries composed ofneutron stars and/or black holes to a fiducial distance of ~200 Mpc and alocalization region of ~100 sq. deg. To maximize the science gains from such GWdetections it is essential to identify electromagnetic (EM) counterparts. Themost promising such counterpart is optical/IR emission powered by theradioactive decay of r-process elements synthesized in the neutron-rich mergerejecta - a "kilonova". Here we present detailed simulated observations thatencompass a range of strategies for kilonova searches during GW follow-up. Weassess both the detectability of kilonovae and our ability to distinguish themfrom a wide range of contaminating transients. We find that if pre-existingtemplate images for the localization region are available, then nightlyobservations to a depth of i=24 mag and z=23 mag are required to achieve a 95%detection rate; observations that commence within 12 hours of trigger will alsocapture the kilonova peak and provide stronger constraints on the ejectaproperties. We also find that kilonovae can be robustly separated from othertypes of transients utilizing cuts on color (i-z > 0 mag) and rise time (< 4days). In the absence of a pre-existing template the observations must reach ~1mag deeper to achieve the same kilonova detection rate, but robust rejection ofcontaminants can still be achieved. Motivated by the results of our simulationswe discuss the expected performance of current and future wide-field telescopesin achieving these observational goals, and find that prior to LSST the DarkEnergy Camera on the Blanco 4-m telescope and Hyper Suprime-Cam on the Subaru8-m telescope offer the best kilonova discovery potential.

A Comprehensive Study of Detectability and Contamination in Deep Rapid Optical Searches for Gravitational Wave Counterparts