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We present detailed simulations of black hole-neutron star (BH-NS) mergerskilonova and gamma-ray burst (GRB) afterglow and kilonova luminosity function,and discuss the detectability of electromagnetic (EM) counterpart in connectionwith gravitational wave (GW) detections, GW-triggered target-of-opportunityobservations, and time-domain blind searches. The predicted absolute magnitudeof the BH-NS kilonovae at $0.5\,{\rm days}$ after the merger falls in$[-10,-15.5]$. The simulated luminosity function contains the potentialviewing-angle distribution information of the anisotropic kilonova emission. Wesimulate the GW detection rates, detectable distances and signal duration, forthe future networks of 2nd/2.5th/3rd-generation GW detectors. BH-NSs tend toproduce brighter kilonovae and afterglows if the BH has a higher aligned-spin,and a less massive NS with a stiffer EoS. The detectability of kilonova isespecially sensitive to the BH spin. If BHs typically have low spins, the BH-NSEM counterparts are hard to discover. For the 2nd generation GW detectornetworks, a limiting magnitude of $m_{\rm limit}\sim23-24\,{\rm mag}$ isrequired to detect the kilonovae even if BH high spin is assumed. Thus, aplausible explanation for the lack of BH-NS associated kilonova detectionduring LIGO/Virgo O3 is that either there is no EM counterpart (plungingevents), or the current follow-ups are too shallow. These observations stillhave the chance to detect the on-axis jet afterglow associated with an sGRB oran orphan afterglow. Follow-up observations can detect possible associated sGRBafterglows, from which kilonova signatures may be studied. For time-domainobservations, a high-cadence search in redder filters is recommended to detectmore BH-NS associated kilonovae and afterglows.

astrophysical journal/the astrophysical journal

Kilonova Emission From Black Hole-Neutron Star Mergers. II. Luminosity  Function and Implications for Target-of-opportunity Observations of  Gravitational-wave Triggers and Blind Searches