Assessing the Readiness of Numerical Relativity for LISA and 3G Detectors
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.
Keywords
Cite
@article{arxiv.2006.04272,
title = {Assessing the Readiness of Numerical Relativity for LISA and 3G Detectors},
author = {Deborah Ferguson and Karan Jani and Pablo Laguna and Deirdre Shoemaker},
journal= {arXiv preprint arXiv:2006.04272},
year = {2021}
}
Comments
7 pages, 5 figures