Raw fluxes uncorrected for the breathing effect (empty disks), as a function of time, relative to the center of the planetary transit. After correction by the f_breath function in Visits 1 and 3 (filled squares), the fluxes within a given orbit are, on average, equal to the best-fit value obtained for F_nom in this orbit. Each point stands for a 300 s exposure spectrum summed over the whole Lyman-α line. Vertical dotted lines show the beginning and end of ingress and egress of the transit. The color code is the same as in Fig. 1, and Visits 1, 2, and 3 are displayed from top to bottom.