Illustration of the physical evolution of SN 2018bsz assuming a scenario of disk-like CSM surrounding an H-poor star. Observer is assumed to be on the left as marked in the first panel. (a) System before the explosion. (b) Upon the explosion the ejecta quickly overtakes a significant part of the disk hiding the CSM emission lines. Only the faint blue component is possibly present. (c) As the ejecta photosphere recedes, the CSM starts to re-emerge and multi-component emission becomes visible. At this stage the photosphere is CSM-driven. (d) CSM on the near-side has completely re-emerged causing the photosphere to recede and the blue component to fade. The CSM disk is represented with cones and ejecta with a sphere for simplicity. The photosphere is marked by dashed red line.