Left: WASP-43 b occultation photometry, binned per intervals of 2 min, period-folded on the best-fit transit ephemeris deduced from our global MCMC analysis (see Sect. 3.3), and shifted along the y-axis for clarity. The best-fit baseline+occultation models are superimposed on the light curves (blue = TRAPPIST z′-filter; green = VLT/HAWK-I NB1190 filter; red = VLT/HAWK-I NB2090 filter). Right: same light curves divided by their best-fit baseline models. The corresponding best-fit occultation models are superimposed.