2008/03/04 by M. Valdés, Andrea Ferrara, A. Ferrara
Physics and Astronomy · #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2008.00471.x
Accepted for publication in MNRAS Letters, 5 pages, 2 figures, 1 table
arxiv created 2008/03/04 · openalex publication_date 2008/05/05 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Abstract We use a set of Monte Carlo simulations to follow the cascade produced by a primary electron of energy Ein in the intergalactic medium. We choose Ein= 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 Lyα resonance and those with energy E < 10.2 eV that do not interact further with gas. This separation is important because a Lyα 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.