  The gravitational wave signal emitted during the coalescence of two neutron
stars carries information about the stars' internal structure. During the long
inspiral phase the main matter observable is the tidal interaction between the
binary components, an effect that can be parametrically modeled with
compact-binary solutions to General Relativity. After the binary merger the
main observable is frequency modes of the remnant, most commonly giving rise to
a short-duration signal accessible only through numerical simulations. The
complicated morphology and the decreasing detector sensitivity in the relevant
frequencies currently hinder detection of the post-merger signal and motivate
separate analyses for the pre-merger and post-merger data. However, planned and
ongoing detector improvements could soon put the post-merger signal within
reach. In this study we target the whole pre-merger and post-merger signal
without an artificial separation at the binary merger. We construct a hybrid
analysis that models the inspiral with templates based on analytical
calculations and calibrated to numerical relativity and the post-merger signal
with a flexible morphology-independent analysis. Applying this analysis to
GW170817 we find, as expected, that the post-merger signal remains undetected.
We further study simulated signals and find that we can reconstruct the full
signal and simultaneously estimate both the pre-merger tidal deformation and
the post-merger signal frequency content. Our analysis allows us to study
neutron star physics using all the data available and directly test the
pre-merger and post-merger signal for consistency thus probing effects such as
the onset of the hadron-quark phase transition.
