We develop a model for frequency-domain gravitational waveforms from inspiraling binary neutron stars .
Our waveform model is calibrated by comparison with hybrid waveforms constructed from our latest high-precision numerical-relativity waveforms and the SEOBNRv2T waveforms in the frequency range of 10 – 1000 { Hz } .
We show that the phase difference between our waveform model and the hybrid waveforms is always smaller than 0.1 { rad } for the binary tidal deformability , { \tilde { \Lambda } } , in the range 300 \lesssim { \tilde { \Lambda } } \lesssim 1900 and for the mass ratio between 0.73 and 1 .
We show that , for 10 – 1000 { Hz } , the distinguishability for the signal-to-noise ratio \lesssim 50 and the mismatch between our waveform model and the hybrid waveforms are always smaller than 0.25 and 1.1 \times 10 ^ { -5 } , respectively .
The systematic error of our waveform model in the measurement of { \tilde { \Lambda } } is always smaller than 20 with respect to the hybrid waveforms for 300 \lesssim { \tilde { \Lambda } } \lesssim 1900 .
The statistical error in the measurement of binary parameters is computed employing our waveform model , and we obtain results consistent with the previous studies .
We show that the systematic error of our waveform model is always smaller than 20 \% ( typically smaller than 10 \% ) of the statistical error for events with the signal-to-noise ratio of 50 .