Kozai cycles integrated using the Hermite integrator with a time-step parameter of η = 0.001. Initial condition was a binary with masses m₁ = 1M_Jup and m₂ = 1M_⊙ with semimajor axis a₁ = 6 AU and eccentricity e₁ = 0.001 orbited by a third body of mass m₃ = 40M_Jup at a distance a₂ = 100 AU and eccentricity e₂ = 0.6. The initial relative inclination was i_tot = 65°. These initial conditions are identical to Figure 3 of Naoz et al. (2013a). The integration errors in both the energy and the semimajor axis of the inner binary rapidly rise at t ∼ 4 Myr, where the inner binary reaches maximum eccentricity.