Comparison of planet properties from the fiducial simulation and the fiducial simulation with non-zero protoplanet eccentricities. Left: final planet masses against the time at which they migrated across r_domain for the fiducial simulation (black), and for the fiducial simulation accounting for non-zero protoplanet eccentricities e_p in the very inner disk (by setting e_p equal to the disk aspect ratio h in the A-code) (red). Right: same as left panel, but now for final planet water fractions instead of masses. Taking into account non-zero eccentricities in the very inner disk leads to only small variations in the final results.