Origin of ΔN_effas a result of an interaction between dark radiation and dark matter

Abstract

Results from the Wilkinson Microwave Anisotropy Probe (WMAP), Atacama Cosmology Telescope (ACT) and recently from the South Pole Telescope (SPT) have indicated the possible existence of an extra radiation component in addition to the well known three neutrino species predicted by the Standard Model of particle physics. In this paper, we explore the possibility of the apparent extra dark radiation being linked directly to the physics of cold dark matter (CDM). In particular, we consider a generic scenario where dark radiation, as a result of an interaction, is produced directly by a fraction of the dark matter density effectively decaying into dark radiation. At an early epoch when the dark matter density is negligible, as an obvious consequence, the density of dark radiation is also very small. As the Universe approaches matter radiation equality, the dark matter density starts to dominate thereby increasing the content of dark radiation and changing the expansion rate of the Universe. As this increase in dark radiation content happens naturally after Big Bang Nucleosynthesis (BBN), it can relax the possible tension with lower values of radiation degrees of freedom measured from light element abundances compared to that of the CMB. We numerically confront this scenario with WMAP+ACT and WMAP+SPT data and derive an upper limit on the allowed fraction of dark matter decaying into dark radiation.

Dark radiation from particle decay: cosmological constraints and opportunities

“…The minimal velocity of the heavier daughter today is obtained by inserting the lower bounds on δ from Sec. 2.2 into (41). We find…”

Converting nonrelativistic dark matter to radiation

“…[4][5][6]). It is however an interesting possibility that the decay products are new massless or very light states in the dark sector, such that effectively a fraction of DM is converted into relativistic 'dark' radiation (DR) [7][8][9][10][11][12][13][14][15]. Such a conversion has received some interest lately as it has been argued to alleviate a possible tension between measurements of the CMB and large scale structure (LSS) observables [15][16][17][18][19][20][21].…”

New light species and the CMB

“…It is possible to construct models where heavier species mimic the effects of light degrees of freedom through a nonzero presure resulting from non-equilibrium distribution functions[52] 5. There are models where out-of-equilibrium effects such as decays generate a contribution to g *[53][54][55][56][57][58][59][60][61][62], but no generic model-independent statements can be made about such scenarios, so we do not consider them in this work.…”