A single field inflation model with large local non-Gaussianity

By Xingang Chen, H. Firouzjahi, Mohammad Hossein Namjoo, Misao Sasaki. 2013

156 citations recorded by the source corpus.

The detection of a large local form of non-Gaussianity is considered to be able to rule out all single field inflation models. This statement is based on the single field consistency condition. Despite the awareness of some implicit assumptions in the derivation of this condition and the demonstration of corresponding examples that illustrate these caveats, to date there is still no explicit and self-consistent model which can serve as a counterexample to this statement. We present such a model in this letter.

Subfields: Astronomy and Astrophysics, Finance, Oceanography

View Paper: https://www.semanticscholar.org/paper/f53bf482cd7fea06f2765e679197253602d69068

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Xingang Chen
2. Yi Wang
3. A. Banday
4. H. Eriksen
5. M. Liguori
6. F. Hansen
7. J. Fergusson
8. E. Shellard

In Finance

1. E. Shellard
2. Xingang Chen
3. Yi Wang
4. M. Liguori
5. J. Fergusson

In Oceanography

1. Xingang Chen
2. A. Banday
3. H. Eriksen
4. F. Hansen
5. M. Liguori
6. Yi Wang
7. P. Lilje
8. Jean-François Cardoso

Citations in the corpus

• Planck 2018 results. IX. Constraints on primordial non-Gaussianity (2019, background): “…slow-roll, with canonical action and initial conditions) predicts that both the amplitude and scale dependence are of the order of the slow-roll parameters (this is true except in some very particular models, see, e.g., Chen et al. (2013)), i.e., they are small and currently not observable.”
• Primordial black holes from inflation and non-Gaussianity (2018, background): “The non-Gaussianity turns out to be completely local (δφ is basically a massless scalar field on the de Sitter background in the limit ≪ 1 and non-Gaussianity is generated after Hubble radius crossing) [59, 60, 63] 〈 ζ~k1ζ~k2ζ~k3 〉 = 3 · (2π)(3)δ((3))(~k1 + ~k2 + ~k3) [Pζ(k1)Pζ(k2) + two terms] .”
• Inflation, Cosmic Perturbations and Non-Gaussianities (2013, background): “One may further enhance this local non-Gaussianity by considering a small sound speed [162].”
• Revisiting non-Gaussianity from non-attractor inflation models (2017, methodology): “So the main conclusions of [19, 20] remain unchanged.”