Neutralino dark matter and the curvaton

Lemoine, Martin; Martin, Jérôme

doi:10.1103/physrevd.75.063504

Cited by 22 publications

(43 citation statements)

References 27 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, if the inflaton and curvaton decays products differ, then there may be an isocurvature component [21,27]. Finally, the simplest scenario predicts a scale-invariant power asymmetry; the asymmetry has been found at multipole moments ℓ < ∼ 40, but there are claims that it does not extend to higher ℓ [28].…”

Section: Summary and Discussionmentioning

confidence: 99%

A hemispherical power asymmetry from inflation

2008

View full text Add to dashboard Cite

Measurements of CMB temperature fluctuations by the Wilkinson Microwave Anisotropy Probe (WMAP) indicate that the fluctuation amplitude in one half of the sky differs from the amplitude in the other half. We show that such an asymmetry cannot be generated during single-field slow-roll inflation without violating constraints to the homogeneity of the Universe. In contrast, a multi-field inflationary theory, the curvaton model, can produce this power asymmetry without violating the homogeneity constraint. The mechanism requires the introduction of a large-amplitude superhorizon perturbation to the curvaton field, possibly a pre-inflationary remnant or a superhorizon curvatonweb structure. The model makes several predictions, including non-Gaussianity and modifications to the inflationary consistency relation, that will be tested with forthcoming CMB experiments.

show abstract

Section: Summary and Discussionmentioning

confidence: 99%

A hemispherical power asymmetry from inflation

2008

View full text Add to dashboard Cite

show abstract

“…If we compare with the equations of motion established in Ref. [25] in the case where the curvaton can decay into dark matter χ (rather than baryons and anti-baryons), the only difference is that terms like Ω 2 χ or Ω 2 χ,eq are replaced by Ω b Ωb and Ω eq b Ω eq b . Notice that, as a consequence, the evolution of the system does not depend on the chemical potential which cancels out, thanks to the fact that µ b = −µb.…”

Section: Description Of the Modelmentioning

confidence: 99%

“…Even though the decay of curvaton may induce a dark matter -radiation isocurvature mode (see Ref. [25] for a detailed analysis), or a baryon -radiation isocurvature mode, both baryonic and dark matter sector will evolve independently. In this sense, the constraints obtained on dark matter or baryon isocurvature modes give complementary constraints on the physics of curvaton decay.…”

Section: Description Of the Modelmentioning

confidence: 99%

“…In order to establish the gauge-invariant equations of motion, we follow the method of Ref. [25]. It consists in formulating the equations in a covariant way in order to be able to perturb them consistently.…”

Section: Description Of the Modelmentioning

confidence: 99%

“…At the background level, following the approach of Ref. [25], the above situation can be modelled by the following set of equations…”

Section: Description Of the Modelmentioning

confidence: 99%

See 2 more Smart Citations

Curvaton decay into baryons, antibaryons, and radiation

Lemoine¹,

Martin²,

Petit³

2008

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

This paper calculates the amount of baryon/radiation isocurvature fluctuation produced through the decay of a curvaton field. It is shown in particular that if curvaton decay preserves baryon number and the curvaton dominates the energy density at the time of decay, the initial curvaton/radiation isocurvature mode is entirely transfered into a baryon/radiation isocurvature mode. This situation is opposite to that previously studied in three fluid models of curvaton decay; this difference is related to the conservation of the pre-existing baryon asymmetry and to the efficiency of the annihilation of all baryon/anti-baryon pairs produced in the decay. We study in detail the relevant cases in which the curvaton decay preserves or not baryon number and provide analytical and numerical calculations for each situation.

show abstract

The Numerical Treatment of Inflationary Models

Ringeval¹

Lecture Notes in Physics

View full text Add to dashboard Cite

Summary. The precision reached by the recent CMB measurements gives new insights into the shape of the primordial power spectra of the cosmological perturbations. In the context of inflationary cosmology, this implies that the CMB data are now sensitive to the form of the inflaton potential. Most of the current approaches devoted to the derivation of the inflationary primordial power spectra, or to the inflaton potential reconstruction problem, rely on approximate analytical treatments that may break down for exotic models. In this article, we numerically solve the inflationary evolution of both the background and all the perturbed quantities to extract the primordial power spectra exactly. Such a method solely relies on General Relativity and linear perturbation theory. More than providing a tool to test analytical approximations, one may consider, without complications, the treatment of non-standard inflationary models as those involving several fields, eventually nonminimally coupled to gravity.The usefulness of the exact numerical approach to deal with CMB data is illustrated by analysing the WMAP third year data in the context of single field models. For this purpose, we introduce a new inflationary related parameter encoding the basic properties of the reheating era. This reheating parameter has significant observable effects and provides a self-consistency test of inflationary models. As a working example, the marginalised probability distributions of the reheating and potential parameters associated with the small field models are presented.

show abstract

Neutralino dark matter and the curvaton

Cited by 22 publications

References 27 publications

A hemispherical power asymmetry from inflation

A hemispherical power asymmetry from inflation

Curvaton decay into baryons, antibaryons, and radiation

The Numerical Treatment of Inflationary Models

Contact Info

Product

Resources

About