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arXiv · 2006.04272

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

Deborah Ferguson·Karan Jani·Pablo Laguna·Deirdre Shoemaker
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Abstract

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.

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Deborah Ferguson, Karan Jani, Pablo Laguna, Deirdre Shoemaker. 2020-06-07. Assessing the Readiness of Numerical Relativity for LISA and 3G Detectors. https://doi.org/10.1103/physrevd.104.044037

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