Number of synthetically observed planets (left) and period ratios of adjacent planets (right) for the planetary systems after 100 Myr of integration; i.e. after the instability phase. The colours are the same as in Fig. 4. The high-viscosity simulations from Izidoro et al. (2021) produce wider systems after the instabilities compared to the low-viscosity simulations, which is also a consequence of the real number of planets in the systems before instabilities (left in Fig. 4), where more planets are initially present at high viscosities.