Planetary architectures around M dwarfs. Top panels: simulated planetary systems of each simulation of the scenarios that include pebble accretion and low gas disk viscosity for a star of 0.1 M_⊙ (left), 0.3 M_⊙ (middle), and 0.5 M_⊙ (right). Bottom panels: observed planetary systems around different stellar masses: 0.08 < M_★/M_⊙ < 0.2 (left), 0.2 < M_★/M_⊙ < 0.4 (middle), and 0.4 < M_★/M_⊙ < 0.5 (right). Planets are discriminated by their masses (as in Figure 4): pM_p < 1 M_⊕ (blue dots), 1 < M_p/M_⊕ < 2 (red dots), 2 < M_p/M_⊕ < 5 (green dots), 5 < M_p/M_⊕ < 10 (orange dots), and M_p/M_⊕ < 20 (black dots). From left to right, panels in the same column present simulated and observed planetary systems around stars with analogous masses for better comparison.