MCMC posterior for the best-fitting, strictly resonant model derived for m_⋆ = 1.47 M_Sun. Parameters included in the diagram are for the planet masses and orbital period ratio κ = P_d/P_e = κ, and parallax Π, inclination I, and the nodal angle Ω (the orbital scale ρ, PO epoch shift t₀ and the common rotation angle ω_rot in the orbital planet are skipped). The crossed lines mark the best-fitting PO solution in terms of the smallest χ² that was used as a starting point to initiate the emcee walkers; see Tables 6 and 7 (Model 1) for parameters of this solution. Uncertainties for the parameters are determined as the 16th and 86th percentile of the samples around the median values.