XMM-Newton (MOS1 – black data points in the electronic version and MOS2 – red data points in the electronic version) unfolded spectrum of IRAS 04507+0358 fitted with a Compton-thin (left panel) and a Compton-thick model (right panel). In the lower panels the ratio between data and best-fit models are shown. In the Compton-thin hypothesis, the data are best reproduced by two thermal emission components (a), b)) plus a power-law absorbed only by the Galactic column density (scattering component, c)) and a power-law absorbed by a high column density (N_H = (4 ± 2)  ×  10²³ cm^-2) absorber e). The two power-laws have the same Γ fixed to 1.9. A prominent iron line is also present d). A similarly good fit could be obtained by using a cold reflection component instead of the absorbed power-law (component e) in the right panel).