Assessing the accuracy limitations of existing waveforms on the data analysis of potential LISA sources.

Future detectors such as LISA will have unprecedented sensitivities enabling us to detect binary black hole coalescences with relatively high signal-to-noise ratios (SNRs), from hundreds to potentially in the thousands for some sources. With this significant increase in the SNR, it is expected that the current accuracies of numerical relativity (and in turn model) waveforms will not be sufficient and introduce systematic errors. In this talk, we present results from our study on the impact of systematic biases introduced by numerical relativity waveforms and the dependent models on the data analysis of potential LISA gravitational wave sources.