Fig. 6.
Top panel: dependence of the different fractions and their binomial errors reported in Sect. 4 as a function of the magnitude cut. Also indicated is the fraction of stars in the sample that have more than 10 individual BeSS spectra available. Middle panel: comparison between the expected fraction of Be+MS systems and the observed fraction of possible Be+MS candidates. In addition we show the corresponding binomial likelihoods of our findings being the result of chance (see text). Bottom panel: number of missing Be+MS systems as a function of the magnitude cut.
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