Final scheme that represents the possible gas distribution inside the disk and the outflowing halos of Mrk 1486. This scheme is built from the conclusions of our modeling of the Lyα radiative transfer inside the galaxy (Sects. 6 and 7). This figure is similar to the one shown in Fig. 9, but the outflowing halos can be now opened in a conical shape that is defined with a cone angle α. The composite SiII line profile obtained from our COS spectrum indicates a clumpy distribution of gas and dust inside the medium of the galaxy disk. Moreover, the clumps are very likely distributed around the source of photons such as the total covering fraction CF = 1. The external layer of the outflowing halos corresponds to a homogeneous medium of HI and dust. This medium plays the most important role in the Lyα transport (all Lyα photons scatter toward the observer from this region). Clumps of HI and dust may composed the internal part of the halos, but their effect on the Lyα radiative transport is negligible.