Particle decays during the cosmic dark ages
Xuelei Chen, Marc Kamionkowski
TL;DR
The paper investigates whether decaying particles can provide partial ionization of the intergalactic medium during the cosmic dark ages to yield the WMAP-measured optical depth without erasing the acoustic peaks in the CMB. It analyzes energy injection from decays, separating channels that ionize/heat the gas from those that escape as photons, and computes the resulting impact on the CMB power spectra. By comparing against both CMB observations and diffuse X-ray/gamma-ray backgrounds, it delineates parameter regions consistent with current data. The work finds that achieving the required optical depth often induces CMB fluctuations that conflict with observations for lifetimes shorter than the age of the Universe, while longer lifetimes may remain viable.
Abstract
We consider particle decays during the cosmic dark ages with two aims: (1) to explain the high optical depth reported by WMAP, and (2) to provide new constraints to the parameter space for decaying particles. We delineate the decay channels in which most of the decay energy ionizes and heats the IGM gas (and thus affects the CMB), and those in which most of the energy is carried away -- e.g. photons with energies 100 keV < E < 1 TeV -- and thus appears as a contribution to diffuse x-ray and gamma-ray backgrounds. The new constraints to the decay-particle parameters from the CMB power spectrum thus complement those from the cosmic X-ray and gamma-ray backgrounds. Although decaying particles can indeed produce an optical depth consistent with that reported by WMAP, in so doing they produce new fluctuations in the CMB temperature/polarization power spectra. For decay lifetimes less than the age of the Universe, the induced power spectra generally violate current constraints, while the power spectra are usually consistent if the lifetime is longer than the age of the Universe.