Fig. 10
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Upper limits to the presence of planets in the disk around MP Mus as a function of radius. These upper limits are derived using Eq. (6) (Lodato et al. 2019) and the fact that no gaps with width Δ ≥ 5 au are detected in the disk. Three different values are used for the proportionality constant (k) linking the planet Hill radius and the corresponding gap width.
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