The detection and subsequent inference of binary black hole signals rely heavily on the accuracy of the waveform model employed. In the highly nonlinear, dynamic, and strong-field regime near merger, these waveforms can only be accurately modeled through numerical relativity simulations. Considering the precision requirements of next-generation gravitational wave observatories, we present in this paper high-resolution simulations of four nonspinning quasicircular binary black hole systems with mass ratios of 1, 2, 3, and 4, conducted using the gr-athena++ code. We extract waveforms from these simulations using both finite radius and Cauchy characteristic extraction (CCE) methods. Additionally, we provide a comprehensive error analysis to evaluate the accuracy and convergence of the waveforms. Our self-mismatch study shows that the (2, 2) mode of the CCE strains, for the world tube extraction radius of $R=50$, reaches the level of $\sim {10}^{-12}$ mismatch for mass ratios of 1, 2, 3, and $\sim {10}^{-11}$ mismatch for the mass ratio of 4. However, when larger extraction radii are considered or when more modes are included the mismatches increase. These results highlight both the promise and limitations of current simulations in achieving the precision required for upcoming detectors such as Laser Interferometer Space Antenna, Cosmic Explorer, and Einstein Telescope.

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• General relativity
• Gravitational waves
• Classical black holes
• Numerical relativity