Final masses of planets (MP = Mc + Menv) as a function of initial radius r0 and initial time t0 in the disc. The plot features a metallicity of Z = 1.0% in pebbles and an amount of Zdust = 0.1% in micrometer sized dust grains, which is a factor of 5 smaller than in Fig. 4. The different lines inside the plots have the same meaning as in Fig. 4. A lower amount of dust grains results in a colder disc, which reduces the pebble isolation mass in the inner disc and therefore increases the parameter space that allows for the formation of ice giants compared to Fig. 4. In the outer disc, formation of larger bodies is easier compared to Fig. 4, because of the larger pebble size and smaller pebble scale height Hpeb in the outer disc.
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