Final masses of planets as a function of initial radius r0 and initial time t0 in the MMSN with a lifetime of 3 Myr. The lines inside the plots correspond to the same meaning as the lines in Fig. 4. We again use a metallicity of pebbles of Z = 1.0%. In contrast to the disc model of Bitsch et al. (2015), the MMSN disc allows 0.1 AU <rf< 5.0 AU only for a very small amount of parameter space. Either the planets fall close to the central star (rf< 0.1 AU) or they stay outside of 5 AU. On the other hand, the parameter region that allows for the formation of ice giants is greatly increased compared to Fig. 4.
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