Best fit model of the spectroscopic observation of IRAS 23226-3843. The original spectrum is shown using a solid black line, the underlying power-law continuum appears using a dashed black line and the model, that includes the most prominent narrow emission lines and – potentially – broad Balmer lines (highlighted using various colors), is shown in red. The characteristics of the broad Lorentzian profiles used to fit the data are listed in Table 3. On the left is the best-fit model for the Hβ line, while the Hα line model is shown on the right. The bottom panels present the residuals (observed spectrum minus the model) for each of the two regions.