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We present numerical relativity simulations of nine-orbit equal-mass binaryneutron star covering the quasicircular late inspiral and merger. The extractedgravitational waveforms are analyzed for convergence and accuracy. Second orderconvergence is observed up to contact, i.e. about 3-4 cycles to merger; errorestimates can be made up to this point. The uncertainties on the phase and theamplitude are dominated by truncation errors and can be minimized to 0.13 radand less then 1%, respectively, by using several simulations and extrapolatingin resolution. In the latter case finite-radius extraction uncertainties becomea source of error of the same order and have to be taken into account. Thewaveforms are tested against accuracy standards for data analysis. Theuncertainties on the waveforms are such that accuracy standards are genericallynot met for signal-to-noise ratios relevant for detection, except for some bestcases using extrapolation from several runs. A detailed analysis of the errorsis thus imperative for the use of numerical relativity waveforms from binaryneutron stars in quantitative studies. The waveforms are compared with thepost-Newtonian Taylor T4 approximants both for point-particle and including theanalytically known tidal corrections. The T4 approximants accumulatesignificant phase differences of 2 rad at contact and 4 rad at merger,underestimating the influence of finite size effects. Tidal signatures in thewaveforms are thus important at least during the last six orbits of the mergerprocess.

Accuracy of numerical relativity waveforms from binary neutron star mergers and their comparison with post-Newtonian waveforms