Eccentricity of the innermost giant planet (left panel) and dust-to-stellar flux ratio at 70 μm after 1 Gyr of evolution (right panel) as a function of the fractional error in the system’s energy budget dE/E. This plot is only for systems with minimum giant planet perihelia of less than 2 AU (see Fig. 22). Our energy error cutoff at 0.01 is shown with the dashed line. There is no evidence for contamination of our sample.