Corner plot of the first eclipse with the pixel-fitting method. Many parameters appear independent but we still find the eclipse depth is correlated with the detector settling parameters h_ramp and l_ramp, similar to Figure I.1. In addition, when the shared height scale of independent pixel systematics h_IPS;shared is high, the height scale of flux-conserving systematics h_FCS is reduced. This makes sense as the "bumps" seen in each pixel light curve in Figure 1 could in principle be fit as either flux-conserved systematics or independent systematics, but the model does clearly prefer to fit a non-zero flux-conserving systematics height scale h_FCS while h_IPS;shared is consistent with zero. This means the model favours that these "bumps" are flux-conserving and not independent.