Waveform systematics in gravitational-wave inference of signals from binary neutron star merger models incorporating higher-order modes information

Accurate information from gravitational wave signals from coalescing binary neutron stars (BNSs) provides essential input to downstream interpretations, including inference of the neutron star population and equation of state. However, even adopting the currently most accurate and physically motivated models available for parameter estimation of BNSs, these models remain subject to waveform modeling uncertainty: differences between these models may introduce biases in recovered source properties. In this work, we describe injection studies investigating these systematic differences between the two best waveform models available for BNSs currently, NRHybSur3dq8Tidal and TEOBResumS. We demonstrate that, for BNS sources observable by current second-generation detectors, differences for low-amplitude signals are significant for certain sources.