Results of our search for variations in the intensity of the observed neutral iron lines. Upper panel: 100 draws from the posterior for scaling factors as a function of phase obtained by fitting models IE (orange), 4E (blue), L (black), Loff (red) and Lbase (green) to the data. The phase coverage of the data is shown in the lower panel, in terms of the S/N of stellar spectra in each phase bin (HARPS-N: lighter pink; CARMENES: darker purple). Where multiple nights cover the same orbital phase bin, their contributions are summed in quadrature.