Posteriors of our orbit analysis of Kepler-444 without including the observed BC−A relative RV. The corresponding credible intervals and the best-fit values of these parameters are listed in Table 6. Fitted parameters are shown as the y-axis in the first eight rows of the corner plot, and the y-axis of the last row presents ΔRV_BC−A,ref, which is the calculated BC−A relative RV at the epoch of 2,456,783.1 JD (i.e., the mean epoch of our observed ΔRV_BC−A value; Section 3.4). There are two families of orbital solutions, with one predicting positive ΔRV_BC−A,ref values and the other predicting negative ΔRV_BC−A,ref values. These two families of solutions have symmetric a, e, and i posteriors against ΔRV_BC−A,ref = 0, but their Ω, ω _⋆, and λ _ref,⋆ posteriors are bimodal, suggesting completely different three-dimensional orientations. The MCMC chains with ΔRV_BC−A,ref ≈ −3.1 km s⁻¹ (horizontal dashed line) correspond to our fitted orbits in Section 4. At the top right, we show that the two families of solutions with different signs of ΔRV_BC−A,ref have comparable posterior probabilities, although their MCMC sample sizes are very different.