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Fig. C.1


Probability density functions of the frequencies of substellar companions around BA (left) and M (right) stars based on the parametric model, computed for companions with semi-major axes in the range a = 5–300 au (plain line) or a = 10–300 au (dashed line), and using the BEX-COND-hot evolutionary tracks for the mass conversion of the detection limits. The same plot for FGK stars is shown in Fig. 8.

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