Frequency-domain gravitational waveform models for inspiraling binary neutron stars
Frequency-domain gravitational waveform models for inspiraling binary neutron stars
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DOI：
10.1103/physrevd.97.044044
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发表时间：
2018-02
影响因子：
5
通讯作者：
K. Kawaguchi;K. Kiuchi;K. Kyutoku;Y. Sekiguchi;M. Shibata;K. Taniguchi
中科院分区：
文献类型：
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作者：
K. Kawaguchi;K. Kiuchi;K. Kyutoku;Y. Sekiguchi;M. Shibata;K. Taniguchi
我们开发了一个来自激励双中子星的频域重力波形模型。我们的波形模型是通过与我们最新的高精度数字相对论波形和频率范围为10-1000 Hz的SEOBNRv2T波形构建的混合波形进行比较来校准的。我们发现，当二元潮汐变形能力Λ ~在300≤Λ ~≤1900范围内，质量比在0.73 ~ 1之间时，我们的波形模型与混合波形之间的相位差始终小于0.1 rad。我们发现，在10-1000 Hz范围内，信号噪声比≤50的可分辨性以及波形模型与混合波形之间的不匹配始终分别小于0.25和1.1×10-5。我们的波形模型在测量Λ ~时，相对于300≤Λ ~≤1900的混合波形，系统误差总是小于20。利用我们的波形模型计算了二值参数测量的统计误差，得到了与前人研究一致的结果。我们表明，对于信噪比为50的事件，我们的波形模型的系统误差总是小于统计误差的20%（通常小于10%）。
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 Λ˜ in the range 300≲Λ˜≲1900 and for a mass ratio between 0.73 and 1. We show that, for 10–1000 Hz, the distinguishability for the signal-to-noise ratio ≲50 and the mismatch between our waveform model and the hybrid waveforms are always smaller than 0.25 and 1.1×10-5, respectively. The systematic error of our waveform model in the measurement of Λ˜ is always smaller than 20 with respect to the hybrid waveforms for 300≲Λ˜≲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 a signal-to-noise ratio of 50.