  Gravitational waves provide us with an extraordinary tool to study the matter
inside neutron stars. In particular, the postmerger signal probes an extreme
temperature and density regime and will help reveal information about the
equation of state of supranuclear-dense matter. Although current detectors are
most sensitive to the signal emitted by binary neutron stars before the merger,
the upgrades of existing detectors and the construction of the next generation
of detectors will make postmerger detections feasible. For this purpose, we
present a new analytical, frequency-domain model for the
inspiral-merger-postmerger signal emitted by binary neutron stars systems. The
inspiral and merger part of the signals are modeled with IMRPhenomD_NRTidalv2,
and we describe the main emission peak of postmerger with a three-parameter
Lorentzian, using two different approaches: one in which the Lorentzian
parameters are kept free, and one in which we model them via quasi-universal
relations. We test the performance of our new complete waveform model in
parameter estimation analyses, studying simulated signals obtained from both
our developed model and by injecting numerical relativity waveforms. We
investigate the performance of different detector networks to determine the
improvement that future detectors will bring to our analysis. We consider
Advanced LIGO+ and Advanced Virgo+, KAGRA, and LIGO-India. We also study the
possible impact of a detector with high sensitivity in the kilohertz band like
NEMO, and finally we compare these results to the ones we obtain with
third-generation detectors, the Einstein Telescope and the Cosmic Explorer.
