Sketch of the three pieces of evidence for elevated ices in HH 48 NE. The orange line demonstrates the effect of including the ices high up in the disk on the vertical absorption profile (panel 1), the relative strength of the 4.3 to 15 μm CO₂ features (panel 2), and the scattering wing of the 4.3 μm CO₂ feature (panel 3). Two scenarios are proposed: a dusty disk wind blocking part of the UV emission from the star (Scenario A) or vertical mixing stirring up ice to the surface (Scenario B).