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Fig. 10


Top panel: distribution of periods as a function of stellar mass for h Per photometric binary candidates (red circles) and for h Per candidate members lying on the cluster’s single-star photometric sequence (blue crosses). Bottom panels: cumulative distribution of periods for photometric binaries and single stars in two mass ranges (left: M ≥ 1.2 M; right: M < 1.2 M). In the two mass bins, there is a clear excess of short period binaries compared to short period single stars (see text).

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