Accuracy of numerical relativity waveforms from binary neutron star
  mergers and their comparison with post-Newtonian waveforms
  We present numerical relativity simulations of nine-orbit equal-mass binary
neutron star covering the quasicircular late inspiral and merger. The extracted
gravitational waveforms are analyzed for convergence and accuracy. Second order
convergence is observed up to contact, i.e. about 3-4 cycles to merger; error
estimates can be made up to this point. The uncertainties on the phase and the
amplitude are dominated by truncation errors and can be minimized to 0.13 rad
and less then 1%, respectively, by using several simulations and extrapolating
in resolution. In the latter case finite-radius extraction uncertainties become
a source of error of the same order and have to be taken into account. The
waveforms are tested against accuracy standards for data analysis. The
uncertainties on the waveforms are such that accuracy standards are generically
not met for signal-to-noise ratios relevant for detection, except for some best
cases using extrapolation from several runs. A detailed analysis of the errors
is thus imperative for the use of numerical relativity waveforms from binary
neutron stars in quantitative studies. The waveforms are compared with the
post-Newtonian Taylor T4 approximants both for point-particle and including the
analytically known tidal corrections. The T4 approximants accumulate
significant phase differences of 2 rad at contact and 4 rad at merger,
underestimating the influence of finite size effects. Tidal signatures in the
waveforms are thus important at least during the last six orbits of the merger
process.
