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Fig. B.1
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Atmospheric C/H, O/H, N/H, C/O, and H2O/H content of planets forming at 3.5, 10, and 30 au in disks with different viscosities. Symbols and color codings are the same as in Fig. 2. We do not take the evaporation of inward drifting pebbles into account, in contrast to Fig. 2, resulting in typically subsolar abundances.
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