Best-fit parameters for the slab model fits to the DF Tau spectrum. Error bars, which are smaller than the points in some cases, are the 3σ confidence intervals of the posterior distributions; the full posteriors are available in Fig. D.1. The sublimation radii R_CO (broad component) and $R_{{\mathrm{H}}_2\mathrm{O}}$ (derived from the IRTF-iSHELL observations) and the dust radii from VLTI-GRAVITY and ALMA are shown with the labeled black lines. As the JWST data are spectrally and spatially unresolved, only the emitting area can be determined; therefore, while the points for the molecular emission in the right panel may be true disk radii, they could also instead represent an annulus farther out with the same emitting area.