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Fig. 26


Top panel: projected eccentricity, measured by the deviation | μ2μ1−0.5 | of the eclipse separation in phase with respect to 0.5, versus orbital period for all sources with and that have two significant eclipse candidates in their two-Gaussian model (with the criterion ΔEcl1BIC > 50 and ΔEcl2BIC > 50). Bottom panel: same as the top figure, but zoomed on short orbital periods on a linear scale.

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