Dynamical excitation of the planetesimal disk after the formation and migration of V1298 Tau b and e in scenario 9 from Table 3. Left panel: Eccentricity. Right panel: inclination. The empty circles in the panels mark the initial position of the giant planets. The simulation stopped with the giant planets about three times more distant from V1298 Tau than their current orbits to prevent dynamical instabilities that would result in a system incompatible with V1298 Tau’s compact architecture.