Equivalently to Fig. 1, but around 1.05 μm. From top to bottom, WASP-33’s pulsations and secondary eclipse, the secondary eclipse once the pulsations have been removed, and the residual light curve once the secondary eclipse is removed. Black continuous lines show best-fit models for the pulsations and the secondary eclipse. Pink and green eclipse models correspond to Deming et al. (2012)’s predicted eclipse depths for inverted and non-inverted atmospheric structures integrated in the Y-band.