Frequency-domain gravitational waveform models for inspiraling binary neutron stars

Abstract

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 $10$--$1000\mathrm{Hz}$. We show that the phase difference between our waveform model and the hybrid waveforms is always smaller than $0.1\mathrm{rad}$ 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 $10$--$1000\mathrm{Hz}$, 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 $50$.

22 pages, 16 figures, accepted for publication in PRD

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• Uncertainty limits on neutron star radius measurements with gravitational waves
• New and Robust Gravitational-Waveform Model for High-Mass-Ratio Binary Neutron Star Systems with Dynamical Tidal Effects
• Second release of the CoRe database of binary neutron star merger waveforms
• The sum of Love: Exploring the effective tidal deformability of neutron stars
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• Unraveling information about supranuclear-dense matter from the complete binary neutron star coalescence process using future gravitational-wave detector networks
• Astrophysical Implications of Neutron Star Inspiral and Coalescence
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• Post-Newtonian templates for gravitational waves from compact binary inspirals
• Discrepancy in tidal deformability of GW170817 between the Advanced LIGO twin detectors
• Gravitational wave constraints on Einstein-æther theory with LIGO/Virgo data
• $f$-mode Imprints in Gravitational Waves from Coalescing Binaries involving Aligned Spinning Neutron Stars
• New gravitational waveform model for precessing binary neutron stars with double-spin effects
• Improving the convergence order of binary neutron star merger simulations in the Baumgarte-Shapiro-Shibata-Nakamura formulation
• Multipole tidal effects in the post-Newtonian gravitational-wave phase of compact binary coalescences
• Black-Hole Neutron Star Simulations with the BAM code: First Tests and Simulations
• Phenomenological model of gravitational self-force enhanced tides in inspiralling binary neutron stars
• High-accuracy high-mass ratio simulations for binary neutron stars and their comparison to existing waveform models
• Follow-up analyses of the binary-neutron-star signals GW170817 and GW190425 by using post-Newtonian waveform models
• Problematic systematics in neutron-star merger simulations
• Modeling matter(s) in SEOBNRv5THM: Generating fast and accurate effective-one-body waveforms for spin-aligned binary neutron stars
• Corrections to the gravitational wave phasing
• Reducing orbital eccentricity in initial data of black hole--neutron star binaries in the puncture framework
• Insights into Binary Neutron Star Merger Simulations: A Multi-Code Comparison
• Auto-encoder model for faster generation of effective one-body gravitational waveform approximations
• Rising Tides: Analytic Modeling of Tidal Effects in Binary Neutron Star Mergers