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Assuming neutron star (NS) or neutron star/stellar-mass black hole (BH)mergers as progenitors of the short gamma ray bursts, we derive and demonstratea simple analysis tool for modelling the efficiency of recovering on-axisoptical afterglows triggered by a candidate gravitational wave event detectedby the Advanced LIGO and Virgo network. The coincident detection efficiency hasbeen evaluated for different classes of operating telescopes using observationsof gamma ray bursts. We show how the efficiency depends on the luminositydistribution of the optical afterglows, the telescope features, and the skylocalisation of gravitational wave triggers. We estimate a plausible opticalafterglow and gravitational wave coincidence rate of 1 yr$^{-1}$ (0.1yr$^{-1}$) for NS-NS (NS-BH), and how this rate is scaled down in detectionefficiency by the time it takes to image the gravitational wave skylocalization and the limiting magnitude of the telescopes. For NS-NS (NS-BH) wefind maximum detection efficiencies of $>80%$ when the total imaging time isless than 200 min (80 min) and the limiting magnitude fainter than 20 (21). Weshow that relatively small telescopes $(m<18)$ can achieve similar detectionefficiencies to meter class facilities $(m<20)$ with similar fields of view,only if the less sensitive instruments can respond to the trigger and image thefield within 10-15 min. The inclusion of LIGO India into the gravitational waveobservatory network will significantly reduce imaging time for telescopes withlimiting magnitudes $\sim20$ but with modest fields of view. An optimalcoincidence search requires a global network of sensitive and fast responsewide field instruments that could effectively image relatively largegravitational-wave sky localisations and produce transient candidates forfurther photometric and spectroscopic follow-up.

The detection efficiency of on-axis short gamma ray burst optical afterglows triggered by aLIGO/Virgo