Top: global line profile (i.e. combining the contributions from the WD’s accretion disc and the Be decretion disc and accounting for the full array of transitions) for our default non-magnetic WD model, at two opposite quadrature orbital phases. The profiles are shown as histograms with energy bins of 1 eV. Bottom: convolution of the global line profiles with an instrumental response function of 5 eV FWHM. The insert displays a zoom on the energy range 6480–6420 eV, to highlight the ~2.6 eV shift between the profiles at the extreme orbital phases. The magenta lines yield the theoretical energies of the centroids of the FeV Kαl and Kα2 subgroups.