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Fig. 18


Comparison of mass functions for two different models and starting times (the detection probability of Mayor et al. (2011) is applied for both panels). Top panel: represents the model computing the internal structure equations. It shows that decreasing the starting time of the embryos, for instance from 1.5 to 1 Myr, allows the appearance of some giants. Bottom panel: represents the B15b approach. We see here that decreasing the starting time of the embryos does not have a significant impact since mainly giant planets formed with this model.

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