Fig. 2
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Cumulative distributions of initial conditions and resulting quantities for different M⋆. The Monte Carlo parameters [Fe/H] and Mgas can be converted to initial solid disk masses (Msolid = 10[Fe∕H]fdg,⊙Mgas, where fdg,⊙ = 0.0149 following Lodders 2003) and disk truncation radii (
, following Andrews et al. 2010). We chose to distribute [Fe/H] equally for all host star masses.
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