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Short, hard gamma-ray bursts (GRBs) are believed to originate from thecoalescence of two neutron stars (NSs) or a NS and a black hole (BH). If thisscenario is correct, then short GRBs will be accompanied by the emission ofstrong gravitational waves (GWs), detectable by GW observatories such as LIGO,Virgo, KAGRA, and LIGO-India. As compared with blind, all-sky, all-time GWsearches, externally triggered searches for GW counterparts to short GRBs havethe advantages of both significantly reduced detection threshold due to knowntime and sky location and enhanced GW amplitude because of face-on orientation.Based on the distribution of signal-to-noise ratios in candidate compact binarycoalescence events in the most recent joint LIGO-Virgo data, our analyticestimates, and our Monte Carlo simulations, we find an effective sensitivevolume for GRB-triggered searches that is about 2 times greater than for anall-sky, all-time search. For NS-NS systems, a jet angle of 20 degrees, agamma-ray satellite field of view of 10% of the sky, and priors with generallyprecessing spin, this doubles the number of NS-NS short-GRB and NS-BH short-GRBassociations, to ~3-4% of all detections of NS-NSs and NS-BHs. We alsoinvestigate the power of tests for statistical excesses in lists ofsubthreshold events, and show that these are unlikely to reveal a subthresholdpopulation until finding GW associations to short GRBs is already routine.Finally, we provide useful formulas for calculating the prior distribution ofGW amplitudes from a compact binary coalescence, for a given GW detectornetwork and given sky location.

Outlook for detection of GW inspirals by GRB-triggered searches in the Advanced detector era