Model components for the flux-resolved spectra of the deep-dipping interval of Obs. 401 (a, b, and c). We show that the direct and scattered emission (see Fig. 4) dominate for different flux levels. The direct part of the emission is shown in red (solid line), and the halo component is shown in blue (dotted line). The halo contribution in spectra b and a causes the double bumped/flattened shape.