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We construct an efficient frequency domain waveform for generic circularcompact object binaries that include neutron stars. The orbital precession issolved on the radiation reaction timescale (and then transformed to thefrequency domain), which is used to map the non-precessional waveform from thesource frame of the binary to the lab frame. The treatment of orbitalprecession is different from that for precessional binary black holes, as$\chi_{\rm eff}$ is no longer conserved due to the spin-induced quadrupolemoments of neutron stars. We show that the new waveform achieves $\le 10^{-4}$mismatch compared with waveforms generated by numerically evolved precessionfor neutron star-black hole systems for $\ge 90\%$ configurations withcomponent mass/spin magnitude assumed in the analysis and randomized initialspin directions. We expect this waveform to be useful to test the nature of themass-gap objects similar to the one discovered in GW 190814 by measuring theirspin-induced quadrupole moments, as it is possible that these mass-gap objectsare rapidly spinning. It is also applicable for the tests of black holemimickers in precessional binary black hole events, if the black hole mimickercandidates have nontrivial spin-induced quadrupole moments.

Efficient fully precessing gravitational waveforms for binaries with neutron stars