Physics-Informed Priors Improve Gravitational-Wave Constraints on Neutron-Star Matter

Abstract

Gravitational-wave astronomy shows great promise in determining nuclear physics in a regime not accessible to terrestrial experiments. We introduce physics-informed priors constrained by nuclear theory and perturbative Quantum Chromodynamics calculations, as well as astrophysical measurements of neutron-star masses and radii. When these priors are used in gravitational-wave astrophysical inference, we show a significant improvement on nuclear equation of state constraints. Applying these to the first observed gravitational-wave binary neutron-star merger GW170817, the constraints on the radius of a $1.4M_{\odot }$ neutron star improve from $R_{1.4}=12.54_{-1.54}^{+1.05}\mathrm{km}$ to $R_{1.4}=12.11_{-1.11}^{+0.91}\mathrm{km}$ and those on the tidal deformability from ${\tilde{\Lambda }}_{1.186}<720$ to ${\tilde{\Lambda }}_{1.186}=384_{-158}^{+306}$ ($90\%$ confidence intervals) at the events measured chirp mass $\mathcal{M}=1.186M_{\odot }$. We also show these priors can be used to perform model selection between binary neutron star and neutron star-black hole mergers; in the case of GW190425, the results provide only marginal evidence with a Bayes factor $\mathcal{B}\mathcal{F}=1.33$ in favour of the binary neutron star merger hypothesis. Given their ability to improve the astrophysical inference of binary mergers involving neutron stars, we advocate for these physics-informed priors to be used as standard in the literature and provide open-source code for reproducibility and adaptation of the method.

Comments: 9 pages, 5 figures. Submitted to ApjL