Radial velocities (top), EW (middle), and longitudinal magnetic field (bottom) of the He I NC as a function of the stellar phase when considering a stellar rotation period of 7.3 ± 0.2 days and considering the first date of observation as ϕ = 0. When they are not visible, the uncertainties are smaller than the symbol. The dotted black lines illustrate the best fits we obtained, with a simple sine (middle and bottom) and the model of Pouilly et al. (2021; top). The color code is the same as in Fig. 1.