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Gravitational waves emitted during the coalescence of binary neutron starsystems carry information about the equation of state describing the extremelydense matter inside neutron stars. In particular, the equation of statedetermines the fate of the binary after the merger: a prompt collapse to blackhole, or the formation of a neutron star remnant that is either stable orsurvives up to a few seconds before collapsing to a black hole. Determining theevolution of a binary neutron star system will therefore place strongconstraints on the equation of state. We present a morphology-independentmethod, developed in the framework of the coherentWaveBurst analysis of signalsfrom ground-based interferometric detectors of gravitational waves. The methodcharacterizes the time-frequency postmerger gravitational-wave emission from abinary neutron star system, and determines whether, after the merger, it formeda remnant neutron star or promptly collapsed to a black hole. We measure thefollowing quantities to characterize the postmerger emission: ratio of signalenergies and match of luminosity profile in different frequency bands, weightedcentral frequency and bandwidth. From these quantities, based on the study ofsignals simulated through injections of numerical relativity waveforms, webuild a statistics to discriminate between the different scenarios after themerger. Finally, we test our method on a set of signals simulated with newmodels, to estimate its efficiency as a function of the source distance.

Minimally modeled characterization method of postmerger gravitational wave emission from binary neutron star coalescences