Fig. 2
Near-infrared occultation light-curves of WASP-5 observed on UT Sep 08 2011 (in staring mode). Each panel from top to bottom shows for the J, H and K bands. Top left: raw light-curves overplotted with the best-fit models, which consist of a theoretical light-curve multiplied with a decorrelation function. Top right: light curves after baseline correction. Bottom left: light curves binned every seven minutes for display purposes. Bottom right: residuals of light-curve fitting.
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