δ Vel Aa-Ab expected broadening functions computed for our models. For each star (Aa and Ab), the open dots are for the model (Table 3) and the thick line is for the analytical function resulting from the fit to the spectroscopic data (Fig. 2). The small gray dots are for the model as well, but ignoring the gravity darkening. In the small panels we plot the residuals “model” – ”fit on spectroscopic data”, where the dashed line is the best fit of the model using the same analytical function, showing the slight underestimation of the gravity darkening by our model.