Precise and accurate neutron star radius measurements with next-generation gravitational wave detectors

Gravitational waves from merging binary neutron stars carry characteristic information about their astrophysical properties, including component masses and tidal deformabilities, that are needed to infer their radii. In this study, we use Bayesian inference to quantify the precision with which radius can inferred with upgrades in the current gravitational wave detectors and next-generation observatories such as the Einstein Telescope and Cosmic Explorer. We assign evidences for a set of plausible equations of state, which are then used as weights to obtain radius posteriors. We find that prior choices and the loudness of observed signals limit the precision and accuracy of inferred radii by current detectors. In contrast, next-generation observatories can resolve the radius precisely and accurately, across most of the mass range to within ≲5% for both soft and stiff equations of state. We also explore how the choice of neutron star mass prior can influence the inferred masses and, in turn, potentially affect radius measurements. However, we find that using an astrophysically motivated prior does not significantly impact the radius measurement of an individual neutron star.