The energy cascade from warm dark matter decays

We use a set of Monte Carlo simulations to follow the cascade produced by a primary electron of energy E-in in the intergalactic medium. We choose E-in = 3-10 keV as expected from the decay of one of the most popular warm dark matter (WDM) candidates, sterile neutrinos. Our simulation takes into account processes previously neglected such as free-free interactions with ions and recombinations, and uses the best available cross-sections for collisional ionizations and excitations with H and He and for electron-electron collisions. We precisely derive the fraction of the primary electron energy that heats the gas, ionizes atoms and produces line and continuum photons as a function of the ionization fraction. Handy fitting formulae for all the above energy depositions are provided. By keeping track of the individual photons, we can distinguish between photons in the Ly alpha resonance and those with energy E < 10.2 eV that do not interact further with gas. This separation is important because a Ly alpha background can heat or cool the gas depending on the nature of the photons, and can have effects on the 21-cm radiation emitted by neutral H, which will probably become detectable at z > 6 in the near future by the next generation radio interferometers.