Combined Hvar V photometry, and HIPPARCOS, KELT, and TESS photometries transformed to V vs. phase of the orbital period, with phase zero corresponding to a conjunction with the Be star behind the secondary according to our orbital solution. This different phase origin is used for convenience because a possible primary eclipse should be observed near phase zero in case of a detached late-type secondary, or near phase 0.5 if the secondary is a compact subdwarf hotter than the Be primary.