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We present a robust method to characterize the gravitational wave emissionfrom the remnant of a neutron star coalescence. Our approach makes only minimalassumptions about the morphology of the signal and provides a full posteriorprobability distribution of the underlying waveform. We apply our method onsimulated data from a network of advanced ground-based detectors anddemonstrate the gravitational wave signal reconstruction. We study thereconstruction quality for different binary configurations and equations ofstate for the colliding neutron stars. We show how our method can be used toconstrain the yet-uncertain equation of state of neutron star matter. Theconstraints on the equation of state we derive are complimentary tomeasurements of the tidal deformation of the colliding neutron stars during thelate inspiral phase. In the case of a non-detection of a post-merger signalfollowing a binary neutron star inspiral we show that we can place upper limitson the energy emitted.

Inferring the post-merger gravitational wave emission from binary neutron star coalescences