Evolution of the inner DM density profiles. Top: density profiles at z = 3, 2, 1.5, 1, 0.5, and 0 for Eris (left) and ErisDark (right). All quantities are plotted in proper units. The black dotted lines indicate the best-fitting modified Burkert profile (see Equation (1)). The location of r ₅₀₀₀, the radius enclosing 5000 DM particles, is indicated with squares. r ₅₀₀₀ corresponds to the density profile convergence radius in ErisDark at z = 0. For Eris the density profile can be trusted to smaller radii due to its larger particle counts, and so we additionally mark r ₁₀₀₀ with a circle. The vertical bars indicate r = 3 _soft. Bottom: the evolution of the logarithmic slope ( dln ρ/ dln  r) measured at different radii: the symbols and thick lines correspond to the slopes at r ₅₀₀₀, and for Eris we also show the slope at r ₁₀₀₀. All lines are boxcar averages over 10 outputs. This plot shows that baryonic physics in Eris leads to the flattening of the central density profile. This flattening appears to be correlated with the growth of the DM offset (see Figure  4). We emphasize that these slopes are not asymptotic slopes, and a value of less than −1 does not imply a strongly cusped profile all the way to the center, but merely indicates the local slope at r ₅₀₀₀, which may lie outside of the scale radius at early times.