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One of the major assumptions in the search for gravitational wave signaturesfrom massive and supermassive black hole binaries with LISA, is that thesesystems will have circularized before entering the LISA bandwidth. Currentastrophysical simulations now suggest that systems could have a non-negligibleeccentricity in the LISA band, and an important level of eccentricity in thePulsar Timing regime. In this work, we use a set of source catalogues fromastrophysically motivated models of massive black hole binary formation andassume a one year LISA mission lifetime. Depending on the model in question,the initial eccentricities in the final year of the inspiral can be as high as0.6 for high mass seeds and 0.8 for low mass seeds. We show that restrictedpost-Newtonian circular templates are extremely inefficient in recoveringeccentric binaries, with median optimal signal to noise ratio recoveries ofapproximately 10% for all models considered. This coupled with extremely largeerrors in parameter recovery from individual Markov chain Monte Carlo'sdemonstrate quite clearly that even to search for binaries with initialeccentricities as low as $10^{-4}$, we will require eccentric templates forLISA data analysis.

Eccentric Massive Black Hole Binaries in LISA I : The Detection Capabilities of Circular Templates