%0 Electronic Article
%A Ng, Sunny
%A Legred, Isaac
%A Suleiman, Lami Shetu
%A Landry, Philippe
%A Traylor, Lyla
%A Read, Jocelyn
%T Inferring the neutron star equation of state with nuclear-physics informed semiparametric models
%N arXiv:2507.03232
%M PUBDB-2026-00595
%M arXiv:2507.03232
%D 2025
%Z 15 pages, 7 figures, matches the published version in Class. Quantum Grav (2025), added figure with sound speed constraints and table with relevant comparisons to other work. Associated Zenodo data release DOI: https://doi.org/10.5281/zenodo.15801144
%X Over the past decade, an abundance of information from neutron-star observations, nuclear experiments and theory has transformed our efforts to elucidate the properties of dense matter. However, at high densities relevant to the cores of neutron stars (NSs), substantial uncertainty about the dense matter equation of state (EoS) remains. In this work, we present a semiparametric EoS framework aimed at better integrating knowledge across these domains in astrophysical inference. We use a meta-model and realistic crust at low densities, and Gaussian process (GP) extensions at high densities. Comparisons between our semiparametric framework to fully nonparametric EoS representations show that imposing nuclear theoretical and experimental constraints through the meta-model up to nuclear saturation density results in constraints on the pressure up to twice nuclear saturation density. We also show that our GP trained on EoS models with nucleonic, hyperonic, and quark compositions extends the range of EoS explored at high density compared to a piecewise polytropic extension schema, under the requirements of causality of matter and of supporting the existence of heavy pulsars (PSRs). We find that maximum Tolman–Oppenheimer–Volkoff masses above 3.2 M<sub>\odot</sub> can be supported by causal EoS compatible with nuclear constraints at low densities. We then combine information from existing observations of heavy PSR masses, gravitational waves emitted from binary NS mergers, and x-ray pulse profile modeling of millisecond PSRs within a Bayesian inference scheme using our semiparametric EoS prior. With information from all public NS Interior Composition ExploRer PSRs (including PSR J0030+0451, PSR J0740+6620, PSR J0437–4715, and PSR J0614–3329), we find an astrophysically favored pressure at two times nuclear saturation density of P(2ρ<sub>nuc</sub>) = 1.98<sup>+2.13</sup><sub>−1.08</sub>×10<sup>34</sup> dyn cm<sup>−2</sup>, a radius of a 1.4 M<sub>\odot</sub> NS value of R<sub>1.4</sub> = 11.4<sup>+0.98</sup><sub>−0.60</sub> km, and M<sub>max</sub> = 2.31<sub>−0.23</sub><sup>+0.35</sup> M<sub>\odot</sub> at the 90
%K neutron stars (autogen)
%K nuclear equation of state (autogen)
%K gravitational waves (autogen)
%K dense matter (autogen)
%K Bayesian inference (autogen)
%K multi-messenger astronomy (autogen)
%F PUB:(DE-HGF)25
%9 Preprint
%R 10.3204/PUBDB-2026-00595
%U https://bib-pubdb1.desy.de/record/645100