Fits of the SEDs of selected programme stars. Each plot consists of two panels. Upper panel: observed fluxes compared to the synthetic SED. To ease the slope of the distribution, the flux f_λ is multiplied by the wavelength to the power of three. Photometric fluxes are displayed as coloured data points with their respective uncertainties and filter widths (dashed lines). The best-fit models are drawn as full-drawn grey lines. Lower panels: uncertainty-weighted residuals χ demonstrating the quality of the fit. The 2200 Å bump in the interstellar extinction curve clearly appears in significantly reddened objects. Top row: He-poor hot subdwarfs (from left to right) – sdB HS2229+2628, sdOB HS2225+2220, and composite sdB pulsator HS1824+5745. Bottom row: single He-sdOB/O stars (from left to right) – eHe sdOB HS1843+6343, eHe sdO HS0019+3944, and iHe-sdO HS1832+6955.