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The discovery of gravitational waves (GW) by Advanced LIGO has ushered usinto an era of observational GW astrophysics. Compact binaries remain theprimary target sources for LIGO, of which neutron star-black hole (NSBH)binaries form an important subset. GWs from NSBH sources carry signatures of(a) the tidal distortion of the neutron star by its companion black hole duringinspiral, and (b) its potential tidal disruption near merger. In this paper, wepresent a Bayesian study of the measurability of neutron star tidaldeformability $\Lambda_\mathrm{NS}\propto (R/M)^{5}$ using observation(s) ofinspiral-merger GW signals from disruptive NSBH coalescences, taking intoaccount the crucial effect of black hole spins. First, we find that ifnon-tidal templates are used to estimate source parameters for an NSBH signal,the bias introduced in the estimation of non-tidal physical parameters willonly be significant for loud signals with signal-to-noise ratios $> 30$. Forsimilarly loud signals, we also find that we can begin to put interestingconstraints on $\Lambda_\mathrm{NS}$ (factor of 1-2) with individualobservations. Next, we study how a population of realistic NSBH detections willimprove our measurement of neutron star tidal deformability. For astrophysicalpopulations of $disruptive$ NSBH mergers, we find 20-35 events to be sufficientto constrain $\Lambda_\mathrm{NS}$ within $\pm 25-50\%$, depending on thechosen equation of state. In this we also assume that LIGO will detect blackholes with masses within the astrophysical $mass$-$gap$. If the mass-gapremains preserved in NSBHs detected by LIGO, we estimate that $25\%$$additional$ detections will furnish comparable tidal measurement accuracy. Inboth cases, we find that the loudest 5-10 events to provide most of the tidalinformation, thereby facilitating targeted follow-ups of NSBHs in the upcomingLIGO-Virgo runs.

Measuring neutron star tidal deformability with Advanced LIGO: a Bayesian analysis of neutron star - black hole binary observations