  Gravitational wave astronomy has established its role in measuring the
equation of state governing cold supranuclear matter. To date and in the near
future, gravitational wave measurements from neutron star binaries are likely
to be restricted to the inspiral. However, future upgrades and the next
generation of gravitational wave detectors will enable us to detect the
gravitational wave signatures emitted after the merger of two stars, at times
when densities beyond those in single neutron stars are reached. Therefore, the
postmerger gravitational wave signal enables studies of supranuclear matter at
its extreme limit. To support this line of research, we present new and updated
phenomenological relations between the binary properties and characteristic
features of the postmerger evolution. Most notably, we derive an updated
relation connecting the mass-weighted tidal deformability and the maximum
neutron star mass to the dominant emission frequency of the postmerger
spectrum. With the help of a configuration-independent Bayesian analysis using
simplified Lorentzian model functions, we find that the main emission frequency
of the postmerger remnant, for signal-to-noise ratios of $8$ and above, can be
extracted within a 1-sigma uncertainty of about 100 Hz for Advanced LIGO and
Advanced Virgo's design sensitivities. In some cases, even a postmerger
signal-to-noise ratio of $4$ can be sufficient to determine the main emission
frequency. This will enable us to measure binary and equation-of-state
properties from the postmerger, to perform a consistency check between
different parts of the binary neutron star coalescence, and to put our physical
interpretation of neutron star mergers to the test.
