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Fig. 8


Upper panel: difference of the binary detection probability, as a function of period, when including or not the four spectra which are not the sum of two exposures (frames 3-2, 4-2, 5-1, and 6-3, see Table 1). For the calculation we assumed an “absolute” criteria with threshold 3.2σ, the same adopted in the present work, and a mean observational error of 3.5 km s-1. Lower panel: detection probability as a function of period, calculated as described in the text. The full and dotted lines indicate the results for the “absolute” criteria with 3.2σ threshold and the “relative” one with 3.8σ criteria, respectively, assuming the typical mean error (3.5 km s-1) of stars cooler than the G1 gap at  ~17 000 K. The results for the “absolute” criteria assuming a mean error of 6.0 km s-1, characteristic of hotter stars, are shown with a dashed line.

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