Spectator Dark Matter

Abstract

The observed dark matter abundance in the Universe can be fully accounted for by a minimally coupled spectator scalar field that was light during inflation and has sufficiently strong self-coupling. In this scenario, dark matter was produced during inflation by amplification of quantum fluctuations of the spectator field. The self-interaction of the field suppresses its fluctuations on large scales, and therefore avoids isocurvature constraints. The scenario does not require any fine-tuning of parameters. In the simplest case of a single real scalar field, the mass of the dark matter particle would be in the range $1\mathrm{GeV}\lesssim m\lesssim 10^8\mathrm{GeV}$, depending on the scale of inflation, and the lower bound for the quartic self-coupling is $\lambda \gtrsim 0.45$.

9 pages, 5 figures. v2: Minor changes, matches the published version

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Cited by in corpus (40)

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• Misalignment & Co.: (Pseudo-)scalar and vector dark matter with curvature couplings
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• Standard model Higgs field and hidden sector cosmology
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• Dark Matter from Entropy Perturbations in Curved Field Space
• Gravitational Wave Symphony from Oscillating Spectator Scalar Fields
• Second-order stochastic theory for self-interacting scalar fields in de Sitter spacetime
• Free scalar correlators in de Sitter via the stochastic approach beyond slow roll
• Spectator dark matter in non-standard cosmologies
• Late vacuum choice and slow roll approximation in gravitational particle production during reheating
• Inflaton freeze-out
• Can dark matter drive electroweak symmetry breaking?
• Estimation of gravitational production uncertainties
• Probing baryogenesis with gravitational waves
• Stochastic isocurvature constraints for axion dark matter with high-scale inflation
• On gravitational preheating