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Extracting the properties of a binary system emitting gravitational wavesrelies on models describing the last stages of the compact binary coalescence.In this article, we study potential biases inherent to current tidal waveformapproximants for spinning and precessing systems. We perform a Bayesian studyto estimate intrinsic parameters of highly spinning binary neutron starsystems. Our analysis shows that one has to include the quadrupolar deformationof the neutron stars due to their rotation once dimensionless spins above $\chi\sim 0.20$ are reached, otherwise the extracted intrinsic parameters aresystematically biased. We find that at design sensitivity of Advanced LIGO andVirgo, it seems unlikely that for GW170817-like sources a clear imprint ofprecession will be visible in the analysis of the signal employing currentwaveform models. However, precession effects might be detectable for unequalmass configurations with spins larger than $\chi>0.2$. We finalize our study byinvestigating possible benefits of a combined gravitational wave andelectromagnetic detection. The presence of electromagnetic counterparts help inreducing the dimensionality of the parameter space with constraints on the skylocation, source distance, and inclination. However, we note that although asmall improvement in the estimation of the tidal deformability parameter isseen in these cases, changes in the intrinsic parameters are overall verysmall.

physical review. d/physical review. d.

Waveform systematics for binary neutron star gravitational wave signals:  Effects of spin, precession, and the observation of electromagnetic  counterparts