Understanding binary neutron star collisions with hypermodels

TL;DR

This paper introduces a hypermodel approach to quantify and compare uncertainties in gravitational-wave models of binary neutron star collisions, revealing systematic differences and aiding future waveform development.

Contribution

It develops a hypermodel technique to measure uncertainties and systematic differences in gravitational-wave approximants for neutron star mergers.

Findings

Identified subtle systematic differences between waveform models.

Detected frequency-dependent effects related to tidal treatment.

Provided a framework for future waveform systematic analysis.

Abstract

Gravitational waves from the collision of binary neutron stars provide a unique opportunity to study the behaviour of supranuclear matter, the fundamental properties of gravity, and the cosmic history of our Universe. However, given the complexity of Einstein's Field Equations, theoretical models that enable source-property inference suffer from systematic uncertainties due to simplifying assumptions. We develop a hypermodel approach to compare and measure the uncertainty gravitational-wave approximants. Using state-of-the-art models, we apply this new technique to the binary neutron star observations GW170817 and GW190425 and the sub-threshold candidate GW200311_103121. Our analysis reveals subtle systematic differences between waveform models, and a frequency-dependence study suggests that this is due to the treatment of the tidal sector. This new technique provides a proving ground for model development, and a means to identify waveform-systematics in future observing runs where detector improvements will increase the number and clarity of binary neutron star collisions we observe.