Planet formation maps with different viscosities for planetary migration using the Jiménez & Masset (2017) formula. Like in Fig. 2, planets that are below the dashed blue line havereached pebble isolation mass and accrete gas. Planets that are interior to the dashed white line have reached runaway gas accretion and can grow very massive. The pebble flux is in all plots. A lower choice of α mostly leads to more massive planets due to the quicker transition to type II migration. In addition, the inwards migration of planets is reduced due to the slow type II migration.