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Fig. 2


Planetary initial mass function at the moment when the gaseous disk disappears. The models do not include any growth processes like giant impacts after disk dispersal, which can significantly modify the mass distribution afterwards, especially for low-mass planets with M ≲ 10   M. Left: PIMF binned according to metallicity. Center: PIMF binned according to the gas disk mass. Left: PIMF binned according to the disk lifetime. The meaning of the different lines, and the limiting values, are indicated in the plot.

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