GLS periodograms of the FHWM (first row) and γ (second row) as computed from the HARPS-N time series after a pre-whitening. Although not always significant, we systematically observe peaks at ∼10d (first column) and ∼6.4d (second column), which we ascribe to the first (P_rot,*/2) and second (P_rot,*/3) harmonics of the stellar rotation period (P_rot,*). A similar behaviour is seen in the other RV-related activity indicators (not shown here).