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Fig. 7


Left: ratio between the dust masses derived in this work and those derived by Ansdell et al. (2016). Although derived with very different methods (for a detailed description, see the text), the masses are within a factor of 2 (gray area) for the vast majority of disks. Right: comparison between the disk inclinations i (along the line of sight) obtained in this work and those derived by Ansdell et al. (2016). In both plots, the disks are sorted from left to right by increasing stellar mass and the circled dots highlight sources with 0.7 ≤ M/M ≤ 1.

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