Left: composite HST image of Haro 11. Image scale is 15 × 15″. East is left, north is up. The Lyα emission is shown in blue, the ionized gas via Hα in red and the UV-continuum in green. The three main star-forming knots A, B and C are labelled. Right: the Lyα vs. the Hα surface brightness for the binned elements in the image. The hatched lines show Lyα = Hα and the case B Lyα/Hα = 8.7. At low surface brightness (1) the theoretical ratio is exceeded due to resonant scattering making the Lyα emission off-set from the ionized regions, while at higher surface brightness; (2) the top edge of the distribution agrees with the recombination value, indicating that the Lyα photons from these regions are scattered just a few times before escaping. Regions with heavy extinction can also be seen at high Hα surface brightnesses (3). The figure is an altered composite of Figs. 3 and 4 in Östlin et al. (2009) (see this article for further information). (A color version of this figure is available in the online journal.)