  Future detectors such as LISA promise signal-to-noise ratios potentially in
the thousands and data containing simultaneous signals. Accurate numerical
relativity waveforms will be essential to maximize the science return. A
question of interest to the broad gravitational wave community is: Are the
numerical relativity codes ready to face this challenge? Towards answering this
question, we provide a new criteria to identify the minimum resolution a
simulation must have as a function of signal-to-noise ratio in order for the
numerical relativity waveform to be indistinguishable from a true signal. This
criteria can be applied to any finite-differencing numerical relativity code
with multiple simulations of differing resolutions for the desired binary
parameters and waveform length. We apply this criteria to binary systems of
interest with the fourth-order MAYA code to obtain the first estimate of the
minimum resolution a simulation must have to be prepared for next generation
detectors.
