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The first direct detection of neutron-star-black-hole binaries will likely bemade with gravitational-wave observatories. Advanced LIGO and Advanced Virgowill be able to observe neutron-star-black-hole mergers at a maximum distanceof 900Mpc. To acheive this sensitivity, gravitational-wave searches will relyon using a bank of filter waveforms that accurately model the expectedgravitational-wave signal. The angular momentum of the black hole is expectedto be comparable to the orbital angular momentum. This angular momentum willaffect the dynamics of the inspiralling system and alter the phase evolution ofthe emitted gravitational-wave signal. In addition, if the black hole's angularmomentum is not aligned with the orbital angular momentum it will cause theorbital plane of the system to precess. In this work we demonstrate that if theeffect of the black hole's angular momentum is neglected in the waveform modelsused in gravitational-wave searches, the detection rate of $(10+1.4)M_{\odot}$neutron-star--black-hole systems would be reduced by $33 - 37%$. The error inthis measurement is due to uncertainty in the Post-Newtonian approximationsthat are used to model the gravitational-wave signal of neutron-star-black-holeinspiralling binaries. We describe a new method for creating a bank of filterwaveforms where the black hole has non-zero angular momentum, but is alignedwith the orbital angular momentum. With this bank we find that the detectionrate of $(10+1.4)M_{\odot}$ neutron-star-black-hole systems would be reduced by$26-33%$. Systems that will not be detected are ones where the precession ofthe orbital plane causes the gravitational-wave signal to match poorly withnon-precessing filter waveforms. We identify the regions of parameter spacewhere such systems occur and suggest methods for searching for highlyprecessing neutron-star-black-hole binaries.

Investigating the effect of precession on searches for neutron-star-black-hole binaries with Advanced LIGO