Correlation plot of the posterior distribution of the eccentricity e and argument of periastron ω of the orbit of WASP-18 b that match the mid-occultation time $T_{\text{occ}}^{\text{JWST}}$ from Coulombe et al. (2023). We used our posterior distribution on planetary parameters from Table 3, and Gaussian priors on e cos ω and e sin ω from Triaud et al. (2010) in blue, Nymeyer et al. (2011) in orange, and Csizmadia et al. (2019) in green. Overall, the 3 posterior distributions are all consistent with each other within <1.2 σ. This plot made use of the package corner.py (Foreman-Mackey 2016).