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Fig. 8


Eclipsing binary light curve for 1SWASP J050634.16–353648.4, over-plotted with the best-fitting model from phoebe. The lower panel shows the residuals between the model fit and the binned data (which we emphasize was not used in the modelling). Around ingress to, and egress from, the primary eclipse, the rapid changes are not as well sampled by the SuperWASP data as in the out-of-eclipse regions, and so give rise to slightly higher residuals of order 0.01 mag.

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