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Fig. E.1.

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Gap depth as a function of planet mass for different disc viscosities at r = 3 AU and 10 AU. Grey bands mark the range of values for fgap that can be generated by zonal flows (Flock et al. 2015). Black dots mark the pebble isolation masses as computed from Bitsch et al. (2018). For α ≤ 3 × 10−4, the pebble isolation masses are in the deep gap regime while higher α results in pebble isolation masses within the shallow gap regime.

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