Fig. 13
Left: dust surface density profiles inferred for all the disks in our Lupus sample (gray curves) compared to the Hayashi (1981) dust surface density model for the solar system (black thick line). The inferred surface density profiles are dashed where they are not spatially resolved, that is for R< 25 au. Right: dust surface density profiles for the sources in the 0.7–1M⊙ stellar mass bin.
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