Non-Gaussian isocurvature perturbations from inflation

Linde, Andrei; Mukhanov, Viatcheslav

doi:10.1103/physrevd.56.r535

Cited by 749 publications

(935 citation statements)

References 19 publications

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“…3 The curvature perturbation ζ is supposed to be negligible when the curvaton starts to oscillate, growing during some radiation-dominated era when ρ σ /ρ ∝ a. After the curvaton decays ζ becomes constant.…”

Section: The Curvature Perturbationmentioning

confidence: 99%

See 1 more Smart Citation

The curvaton as a pseudo-Nambu-Goldstone boson

Dimopoulos

Lyth

Notari

et al. 2003

J. High Energy Phys.

119

128

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The field responsible for the cosmological curvature perturbations generated during a stage of primordial inflation might be the "curvaton", a field different from the inflaton field. To keep the effective mass of the curvaton small enough compared to the Hubble rate during inflation one may not invoke supersymmetry since the latter is broken by the vacuum energy density. In this paper we propose the idea that the curvaton is a pseudo Nambu-Goldstone boson (PNGB) so that its potential and mass vanish in the limit of unbroken symmetry. We give a general framework within which PNGB curvaton candidates should be explored. Then we explore various possibilities, including the case where the curvaton can be identified with the extra-component of a gauge field in a compactified five-dimensional theory (a Wilson line), where it comes from a Little-Higgs mechanism, and where it is a string axion so that supersymmetry is essential.

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Section: The Curvature Perturbationmentioning

confidence: 99%

“…With two exceptions [2,3], the universal assumption until 2001 was that the responsible field was the inflaton, defined in this context as the field whose value determines the end of inflation. Then it was proposed instead [4] that the responsible field is some 'curvaton' 'field different from the inflaton.…”

Section: Introductionmentioning

confidence: 99%

The curvaton as a pseudo-Nambu-Goldstone boson

Dimopoulos

Lyth

Notari

et al. 2003

J. High Energy Phys.

119

128

View full text Add to dashboard Cite

show abstract

“…A simple and even plausible way is to introduce additional light scalars. In the curvaton [14,15,16] and/or ungaussiton [17] scenarios, those light scalars can generate sizable non-Gaussianity [18,19,20]. In the presence of additional light scalars with quantum fluctuations, it is generically expected that isocurvature perturbation may arise.…”

Section: Introductionmentioning

confidence: 99%

“…In the presence of additional light scalars with quantum fluctuations, it is generically expected that isocurvature perturbation may arise. In particular, the non-Gaussianity hinted by the recent observations may originate from a small admixture of isocurvature perturbations [15,21,22].…”

Section: Introductionmentioning

confidence: 99%

A general analysis of non-gaussianity from isocurvature perturbations

Kawasaki

Nakayama

Sekiguchi

et al. 2009

J. Cosmol. Astropart. Phys.

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Light scalars may be ubiquitous in nature, and their quantum fluctuations can produce large non-Gaussianity in the cosmic microwave background temperature anisotropy. The non-Gaussianity may be accompanied with a small admixture of isocurvature perturbations, which often have correlations with the curvature perturbations. We present a general method to calculate the non-Gaussianity in the adiabatic and isocurvature perturbations with and without correlations, and see how it works in several explicit examples. We also show that they leave distinct signatures on the bispectrum of the cosmic microwave background temperature fluctuations.

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“…While the quantum fluctuation of the inflaton is the simplest possibility, there may be many light scalars in nature, which acquire quantum fluctuations extending beyond the horizon during inflation. If so, some of them may give a significant contribution to the observed density perturbations via the curvaton [1][2][3][4] (or its variant, e.g. modulated reheating [5,6]) mechanism.…”

Section: Introductionmentioning

confidence: 99%

The spectral index and its running in axionic curvaton

Takahashi¹

2013

J. Cosmol. Astropart. Phys.

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We show that a sizable running spectral index suggested by the recent SPT data can be explained in the axionic curvaton model with a potential that consists of two sinusoidal contributions of different height and period. We find that the running spectral index is generically, where ∆N is the e-folds during one period of modulations. In the string axiverse, axions naturally acquire a mass from multiple contributions, and one of the axions may be responsible for the density perturbations with a sizable running spectral index via the curvaton mechanism. We note that the axionic curvaton model with modulations can also accommodate the red-tilted spectrum with a negligible running, without relying on large-field inflation.

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Non-Gaussian isocurvature perturbations from inflation

Cited by 749 publications

References 19 publications

The curvaton as a pseudo-Nambu-Goldstone boson

The curvaton as a pseudo-Nambu-Goldstone boson

A general analysis of non-gaussianity from isocurvature perturbations

The spectral index and its running in axionic curvaton

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