2025/05/27 by Soham Mitra, Praveer Tiwari, Mitra, Soham +3
Physics and Astronomy · #Data Analysis #FOS: Physical sciences #Gamma-ray bursts and supernovae #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #High Energy Physics - Phenomenology (hep-ph) #Nuclear Theory (nucl-th) #Pulsars and Gravitational Waves Research #Statistical Mechanics and Entropy #Statistics and Probability (physics.data-an)
paper · pdf · doi:10.48550/arxiv.2505.21667
openalex publication_date 2025/05/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Post-merger gravitational-wave emission from a binary neutron star merger carries crucial information about the equation of state (EoS) of matter at high temperatures. Current gravitational wave detectors have limited sensitivities at post-merger frequencies in the range [1.5, 4] kHz. Therefore, valuable inferences can only be made after combining information from multiple (BNS) events. Criswell et al. [Phys. Rev. D 107, 043021 (2023)] carries out an injection study to infer the radius posterior for a 1.6 M\odot NS by combining the information from injected BNS events via the hierarchical Bayesian inference (HBI) formulation. This formulation utilizes empirical relations that connect the peak frequency of the post-merger remnant with the chirp mass of the system, and the EoS proxy parameter R1.6. In this work, we extend the HBI formulation to other EoS proxy parameters (i.e., the radius of (NS), R1.X, with masses 1.2, 1.4, and 1.8 M\odot) and combine the four R1.X posteriors through the piecewise polytropic EoS model to obtain measurable constraints on the EoS of the NS. We show that the NS radii can be constrained to within ∼1 km ( ∼0.55 km) assuming uniform (astrophysical) prior on R1.X for injections in the A+ noise. We also study systematic biases in the analysis coming from the limitations of empirical relations.