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The recent observation of GW190412, the first high-mass ratio binaryblack-hole (BBH) merger, by the LIGO-Virgo Collaboration (LVC) provides aunique opportunity to probe the impact of subdominant harmonics and precessioneffects encoded in a gravitational wave signal. We present refined estimates ofsource parameters for GW190412 using \texttt{NRSur7dq4}, a recently developednumerical relativity waveform surrogate model that includes all $\ell \leq 4$spin-weighted spherical harmonic modes as well as the full physical effects ofprecession. We compare our results with two different variants ofphenomenological precessing BBH waveform models, \texttt{IMRPhenomPv3HM} and\texttt{IMRPhenomXPHM}, as well as to the LVC results. Our results are broadlyin agreement with \texttt{IMRPhenomXPHM} results and the reported LVC analysiscompiled with the \texttt{SEOBNRv4PHM} waveform model, but in tension with\texttt{IMRPhenomPv3HM}. Using the \texttt{NRSur7dq4} model, we provide atighter constraint on the mass-ratio ($0.26^{+0.08}_{-0.06}$) as compared tothe LVC estimate of $0.28^{+0.13}_{-0.07}$ (both reported as median valueswiths 90\% credible intervals). We also constrain the binary to be moreface-on, and find a broader posterior for the spin precession parameter. Wefurther find that even though $\ell=4$ harmonic modes have negligiblesignal-to-noise ratio, omission of these modes will influence the estimatedposterior distribution of several source parameters including chirp mass,effective inspiral spin, luminosity distance, and inclination. We also findthat commonly used model approximations, such as neglecting the asymmetricmodes (which are generically excited during precession), have negligible impacton parameter recovery for moderate SNR-events similar to GW190412.

Improved analysis of GW190412 with a precessing numerical relativity surrogate waveform model