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The gravitational wave signal emitted during the coalescence of two neutronstars carries information about the stars' internal structure. During the longinspiral phase the main matter observable is the tidal interaction between thebinary components, an effect that can be parametrically modeled withcompact-binary solutions to General Relativity. After the binary merger themain observable is frequency modes of the remnant, most commonly giving rise toa short-duration signal accessible only through numerical simulations. Thecomplicated morphology and the decreasing detector sensitivity in the relevantfrequencies currently hinder detection of the post-merger signal and motivateseparate analyses for the pre-merger and post-merger data. However, planned andongoing detector improvements could soon put the post-merger signal withinreach. In this study we target the whole pre-merger and post-merger signalwithout an artificial separation at the binary merger. We construct a hybridanalysis that models the inspiral with templates based on analyticalcalculations and calibrated to numerical relativity and the post-merger signalwith a flexible morphology-independent analysis. Applying this analysis toGW170817 we find, as expected, that the post-merger signal remains undetected.We further study simulated signals and find that we can reconstruct the fullsignal and simultaneously estimate both the pre-merger tidal deformation andthe post-merger signal frequency content. Our analysis allows us to studyneutron star physics using all the data available and directly test thepre-merger and post-merger signal for consistency thus probing effects such asthe onset of the hadron-quark phase transition.

Probing neutron stars with the full pre-merger and post-merger gravitational wave signal from binary coalescences