Photometry of individual components of the 288P system. The components are identified based on their relative positions according to the orbit models shown in Fig. 5. The component that is brighter in the inactive state is labelled “A”, the fainter one “B”. Panel a: absolute magnitudes of the individual components for those visits where D > 0.04′′. Data from visit 24 are plotted separately for each HST orbit. The areas shaded in violet and green mark the brightness ranges compatible with visits 14–17 + 24, assuming that these are the minimum ranges of their rotational lightcurves. Black circles indicate the tail-sided component for any given time, hence the non-circled components were located in the direction of the Sun. Vertical dashed lines separate 2011 from 2016 visits, and the active from the inactive phase. Panel b: absolute magnitudes during the active phases as functions of heliocentric distance r_h. Numbers label the visit. Within the 2016/17 data set, component B shows a systematic dependency between magnitude and r_h, while A does not.