Fig. 13
Cumulative number of stars per square arcsec, computed from a combined image of the field of CoRoT-24 that is complete down to RG ~25. The two vertical lines correspond to the extremes of the horizontal lines in Fig. 7, i.e., the highest magnitude a star could have in order to reproduce the observed transit depth of CoRoT-24b while completely disappearing during eclipses, and the magnitude of a star with 50% eclipses needed to explain the transit depth of CoRoT-24c.
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