Cosmological Constraints on Decaying Dark Matter

• Published in: arXiv.org 2009-01
• Main Authors: Santiago De Lope Amigo, Cheung, William Man-Yin, Huang, Zhiqi, Siew-Phang Ng
• Format: Article
• Language: English
• Subjects: Astronomical models; Big Bang theory; Confidence intervals; Cosmic microwave background; Cosmology; Dark matter; Ionization; Large scale structure of the universe; Operators; Particle decay; Particle physics; Standard model (particle physics); Supergravity; Supersymmetry
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.0812.4016

We present a complete analysis of the cosmological constraints on decaying dark matter. Previous analyses have used the cosmic microwave background and Type Ia supernova. We have updated them with the latest data as well as extended the analysis with the inclusion of Lyman-\(\alpha\) forest, large scale structure and weak lensing observations. Astrophysical constraints are not considered in the present paper. The bounds on the lifetime of decaying dark matter are dominated by either the late-time integrated Sachs-Wolfe effect for the scenario with weak reionization, or CMB polarization observations when there is significant reionization. For the respective scenarios, the lifetimes for decaying dark matter are \(\Gamma^{-1} \gtrsim 100\) Gyr and \( (f \Gamma) ^{-1} \gtrsim 5.3 \times 10^8\) Gyr (at 95.4% confidence level), where the phenomenological parameter \(f\) is the fraction of the decay energy deposited in baryonic gas. This allows us to constrain particle physics models with dark matter candidates through investigation of dark matter decays into Standard Model particles via effective operators. For decaying dark matter of \(\sim 100\) GeV mass, we found that the size of the coupling constant in the effective dimension-4 operators responsible for dark matter decay has to generically be \( \lesssim 10^{-22}\). We have also explored the implications of our analysis for representative models in theories of gauge-mediated supersymmetry breaking, minimal supergravity and little Higgs.