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With the increasing sensitivity of advanced gravitational wave detectors, thefirst joint detection of an electromagnetic and gravitational wave signal froma compact binary merger will hopefully happen within this decade. However,current gravitational-wave likelihood sky areas span $\sim100-1000\,\textrm{deg}^2$, and thus it is a challenging task to identify which,if any, transient corresponds to the gravitational-wave event. In this study,we make a comparison between recent kilonovae/macronovae lightcurve models forthe purpose of assessing potential lightcurve templates for counterpartidentification. We show that recent analytical and parametrized models forthese counterparts result in qualitative agreement with more complicatedradiative transfer simulations. Our analysis suggests that with improvedlightcurve models with smaller uncertainties, it will become possible toextract information about ejecta properties and binary parameters directly fromthe lightcurve measurement. Even tighter constraints are obtained in cases forwhich gravitational-wave and kilonovae parameter estimation results arecombined. However, to be prepared for upcoming detections, more realistickilonovae models are needed. These will require numerical relativity with moredetailed microphysics, better radiative transfer simulations, and a betterunderstanding of the underlying nuclear physics.

Towards rapid transient identification and characterization of kilonovae