Distributions inferred a posteriori for the activity-related detrending coefficients (i.e. β₀, β_⋅, F, β_⋅, A, and β_⋅, γ of Eq. (1); the digit in the subscript refers to the polynomial order). Each panel compares the optimal detrending coefficients applied to the two different piecewise stationary segments that were found within the HARPS-pre dataset. The difference between the two distributions of each parameter emphasises that stellar activity impacts the RV observations differently when moving from one segment to the other.