Reanalysis of the binary neutron star mergers GW170817 and GW190425 using numerical-relativity calibrated waveform models.

We reanalyze gravitational waves from binary-neutron-star mergers GW170817 and GW190425 using a numerical-relativity (NR) calibrated waveform model, the TF2+_Kyoto model, which includes nonlinear tidal terms. For GW170817, by imposing a uniform prior on the binary tidal deformability $\tilde{\Lambda}$, the symmetric $90\%$ credible interval of $\tilde{\Lambda}$ is estimated to be $481^{+436}_{-359}$ ($402^{+465}_{-279}$) for the case of $f_\mathrm{max}=1000~\mathrm{Hz}$ ($2048~\mathrm{Hz}$), where $f_\mathrm{max}$ is the maximum frequency in the analysis. We also reanalyze the event with other waveform models: two post-Newtonian waveform models (TF2_PNTidal and TF2+_PNTidal), the TF2+_NRTidal model that is another NR calibrated waveform model, and its upgrade, the TF2+_NRTidalv2 model. While estimates of parameters other than $\tilde{\Lambda}$ are broadly consistent among various waveform models, our results indicate that estimates of $\tilde{\Lambda}$ depend on waveform models. However, the difference is smaller than the statistical error. For GW190425, we can only obtain little information on the binary tidal deformability. The systematic error among the NR calibrated waveform models will become significant to measure $\tilde{\Lambda}$ as the number of detectors and events increase and sensitivities of detectors are improved.