Normalised PSF profile around CoRoT-24, from a VLT/NACO combined image. The horizontal lines delimit the flux level that a contaminant included in the CoRoT ’s PSF should reach in order to produce the observed diluted transit depth. Two lines are plotted, for an unrealistic contaminant completely disappearing during eclipse (100% eclipse line), and a 50% eclipse. Dashed line is for CoRoT-24c, while dotted line is for CoRoT-24b. Realistic potential background eclipsing binaries should lie closer than 1.3′′ and 0.9′′ to the main star to explain the transit depths of CoRoT-24b and c, respectively.