Set of posterior PDFs showing the distributions of CMF_planet, the CMF of the planets as measured from their masses and radii (orange), and CMF_star, the equivalent CMF as inferred from the refractory abundances of their host stars (blue), for each planet. Due to the high uncertainty in abundances for some stars, such as GJ 1252, some draws from the posterior are fit with very low [Fe/H] values and very high [Mg/H] and [Si/H] values, resulting in a very low CMF_star, causing a large amount of posterior draws to converge to CMF_star ≈ 0.