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Using the \texttt{lalinference} Markov-chain Monte Carlo parameter estimationcode, we examine two distinct nonprecessing black hole-neutron star (BH-NS)binaries with and without higher-order harmonics. Our simulations suggest thathigher harmonics provide a minimal amount of additional information,principally about source geometry. Higher harmonics do providedisproportionately more information than expected from the signal power. Ourresults compare favorably to the "effective Fisher matrix" approach.Extrapolating using analytic scalings, we expect higher harmonics will providelittle new information about nonprecessing BH-NS binaries at the signalamplitudes expected for the first few detections. Any study of subdominantdegrees of freedom in gravitational wave astronomy can adopt the toolspresented here ($V/V_{\rm prior}$ and $D_{KL}$) to assess whether new physicsis accessible (e.g., modifications of gravity; spin-orbit misalignment) and ifso precisely what information those new parameters provide. Forastrophysicists, we provide a concrete illustration of how well parameters of aBH-NS binary can be measured, relevant to the astrophysical interpretation ofcoincident EM and GW events (e.g., short GRBs). For our fiducialinitial-detector example, the individual masses can be determined to liebetween $7.11-11.48 M_\odot$ and $1.77-1.276M_\odot$ at greater than 99%confidence, accounting for unknown BH spin. Assuming comparable control overwaveform systematics, future measurements of BH-NS binaries can constrain theBH and perhaps NS mass distributions.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d, particles, fields, gravitation, and cosmology

Parameter Estimation of Gravitational Waves from Nonprecessing BH-NS  Inspirals with higher harmonics: Comparing MCMC posteriors to an Effective  Fisher Matrix