  Precision cosmology is crucial to understand the different energy components
in the Universe and their evolution through cosmic time. Gravitational wave
sources are standard sirens that can accurately map out distances in the
Universe. Together with the source redshift information, we can then probe the
expansion history of the Universe. We explore the capabilities of various
gravitational-wave detector networks to constrain different cosmological models
while employing separate waveform models for inspiral and post-merger part of
the gravitational wave signal from equal mass binary neutron stars. We consider
two different avenues to measure the redshift of a gravitational-wave source:
first, we examine an electromagnetic measurement of the redshift via either a
kilonova or a gamma ray burst detection following a binary neutron star merger
(the electromagnetic counterpart method); second, we estimate the redshift from
the gravitational-wave signal itself from the adiabatic tides between the
component stars characterized by the tidal Love number, to provide a second
mass-scale and break the mass-redshift degeneracy (the counterpart-less
method). We find that the electromagnetic counterpart method is better suited
to measure the Hubble constant while the counterpart-less method places more
stringent bounds on other cosmological parameters. In the era of
next-generation gravitational-wave detector networks, both methods achieve
sub-percent measurement of the Hubble constant $H_0$ after one year of
observations. The dark matter energy density parameter $\Omega_{\rm M}$ in the
$\Lambda$CDM model can be measured at percent-level precision using the
counterpart method, whereas the counterpart-less method achieves sub-percent
precision. We, however, do not find the postmerger signal to contribute
significantly to these precision measurements.
