Fig. 4.

Spectra of effective transit height, $z_{\text{eff},\lambda }=R_{\text{eff},\lambda }-R_p$, for all four Cassini/VIMS occultation datasets. Key absorption features are labeled, and error bars are shown only where the 1 − σ uncertainty is larger than 1%. Our best-fit haze model for the 70° S dataset is shown (dashed line).