  We present a robust method to characterize the gravitational wave emission
from the remnant of a neutron star coalescence. Our approach makes only minimal
assumptions about the morphology of the signal and provides a full posterior
probability distribution of the underlying waveform. We apply our method on
simulated data from a network of advanced ground-based detectors and
demonstrate the gravitational wave signal reconstruction. We study the
reconstruction quality for different binary configurations and equations of
state for the colliding neutron stars. We show how our method can be used to
constrain the yet-uncertain equation of state of neutron star matter. The
constraints on the equation of state we derive are complimentary to
measurements of the tidal deformation of the colliding neutron stars during the
late inspiral phase. In the case of a non-detection of a post-merger signal
following a binary neutron star inspiral we show that we can place upper limits
on the energy emitted.
