Reconstructed spectral energy distributions of RR Tel in two epochs: a) 1997/05/15 and b) 1997/11/19, differing in time by a half of the Mira pulsation period. The best-fitted DUSTY model for dust density distribution enhanced by radiatively driven winds is given by the full thick line. Observations in the near-IR are marked by four circles with their corresponding error bars for J, H, K and L wavelengths, while the ISO/SWS observations are shown by the thin full line and cover an interval from 2.3 to 13 μm. The three contributions to the model are: attenuated radiation of the Mira component (dotted line), dust scattering (dashed line), and dust emission (dot-dashed line).