The detection of the gravitational waves produced after the coalescence of two neutron stars is greatly anticipated because it will be able to provide information about matter in extreme conditions, especially if the remnant turns out to go through a hypermassive or a supermassive neutron star state before collapsing into a black hole. Next-generation gravitational wave detectors, such as the Einstein Telescope, the Cosmic Explorer, and the Neutron-star Extreme Matter Observatory are expected to observe high-frequency gravitational wave signals, that is, the postmerger stage of the coalescence of binary neutron stars; then from these signals one can estimate the maximum mass that a spinless neutron star (${\mathrm{M}}_{\mathrm{TOV}}$) can have. In this paper, we investigate the problem of the determination of the ${\mathrm{M}}_{\mathrm{TOV}}$ precision from the postmerger detected by next-generation observatories. Our results show that only under the most optimistic scenario of signal-to-noise ratio for post-merger signals ($\mathrm{SNR}\ge 8$) and merger rate density ($250{\mathrm{Gpc}}^{-3}{\mathrm{yr}}^{-1}$), CE 20 km achieves the highest mass precision in the range $\delta M/2\approx 0.1–0.3M_{\odot }$ for a remnant mass of $2.57M_{\odot }$ in five years of observation. We clarify that this precision represents the minimum uncertainty, corresponding to the most probable value (main peak) in the final mass distribution, showing that it depends on the value of the final (remnant) mass. Therefore, based on the results obtained in this study, it may still be necessary to improve the sensitivity at high frequencies of future ground-based gravitational wave observatories if one wants to obtain greater precision in the estimation of ${\mathrm{M}}_{\mathrm{TOV}}$. One possibility would be to improve the sensitivity in a frequency range that allows us to determine whether or not a black hole was formed or will be formed in the coalescence. The right choice of interferometer length and tunable design that optimizes detection at high frequencies is essential for a successful determination of ${\mathrm{M}}_{\mathrm{TOV}}$. Other lengths and tunable designs of interferometers, as well as sensitivity curves extended up to 10 kHz for both present versions of CE (since the reference used for CE provides these curves only up to 5 kHz), will be considered in future work, seeking to increase the number of postmerger detections in five years of observation and also determine the final merger product.

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• Gravitational waves
• Binary stars
• Neutron stars & pulsars
• Astronomical masses & mass distributions
• Gravitational wave detectors
• Numerical techniques