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

Assessing the Readiness of Numerical Relativity for LISA and 3G Detectors