Comparison between the observed Lyα line profile of Mrk 1486 (blue thick line) and the one escaping from our 3D geometry when assuming an extremely clumpy distribution of HI and dust inside the galaxy disk and the outflowing halos (i.e., with an optically thin interclump medium, n_IC/n_C = 0). The magenta dashed line shows the spectrum that escapes from the galaxy disk. The spectra of wind 1 and wind 2 are shown as a black dotted and a blue dashed-dotted line, respectively. When assuming n_IC/n_C = 0 in each component, we always obtain a strong emission at the Lyα line center.