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The UV escape fraction from high-redshift galaxies plays a key role in modelsof cosmic reionisation. Because it is currently not possible to deduce theescape fractions during the epoch of reionisation from observations, we have torely on numerical simulations. Our aim is to better constrain the escapefraction from high-redshift dwarf galaxies, as these are the most likelysources responsible for reionising the Universe. We employ a N-body/SPH methodthat includes realistic prescriptions for the physical processes that areimportant for the evolution of dwarf galaxies. These models are post-processedwith radiative transfer to determine the escape fraction of ionising radiation.We perform a parameter study to assess the influence of the spin parameter, gasfraction and formation redshift of the galaxy and study the importance ofnumerical parameters as resolution, source distribution and local gas clearing.We find that the UV escape fraction from high-redshift dwarf galaxies that haveformed a rotationally supported disc lie between 1e-5 and 0.1. The mass andangular momentum of the galaxy are the most important parameters that determinethe escape fraction. We compare our results to previous work and discuss theuncertainties of our models. The low escape fraction we find for high-redshiftdwarf galaxies is balanced by their high stellar content, resulting in anefficiency parameter for stars that is only marginally lower than the valuesfound by semi-analytic models of reionisation. We therefore conclude that dwarfgalaxies play an important role in cosmic reionisation also after the initialstarburst phase, when the gas has settled into a disc.

The escape of ionising radiation from high-redshift dwarf galaxies