Primordial Non-Gaussianities from Inflation Models
By Xingang Chen. 2010
663 citations recorded by the source corpus.
This is a pedagogical review on primordial non-Gaussianities from inflation models. We introduce formalisms and techniques that are used to compute such quantities. We review different mechanisms which can generate observable large non-Gaussianities during inflation, and distinctive signatures they leave on the non-Gaussian profiles. They are potentially powerful probes to the dynamics of inflation. We also provide a nontechnical and qualitative summary of the main results and underlying physics.
Subfields: Astronomy and Astrophysics, Oceanography
View Paper: https://www.semanticscholar.org/paper/d7998de1ee52fc215d097f930e2d32b4e5ff8f5d
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Citations in the corpus
- Equilateral Non-Gaussianity and New Physics on the Horizon (2011, neutral): “We will use the in-in formalism to compute correlation functions (for a recent review see [39]) 〈Q̂〉(τ) = 〈0| [ T̄ e ∫ τ −∞ dτ Ĥint(τ ′) ] Q̂(τ) [ T e−i ∫ τ −∞ dτ Ĥint(τ ′) ] |0〉 , (C.”
- Revisiting non-Gaussianity from non-attractor inflation models (2017, background): “Related to this issue, it is also known that the presence of sharp feature on potential will generate scale-dependent oscillatory signals in power spectrum and non-Gaussianities (See e.g. [12] for a review).”
- Planck2018 results (2018, background): “The above parameterization is a proxy for models that contain sharp oscillatory features (Chen 2010; Hu 2011; Adshead & Hu 2014), although typically such effects would generate decaying features, which will not be considered here.”
- Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “(See Chen 2010 and Komatsu 2010 for recent reviews.)”
- Schwinger-Keldysh diagrammatics for primordial perturbations (2017, background): “See [1, 2] for reviews of the canonical in-in formalism.”
- Review of local non-Gaussianity from multi-field inflation (2010, background): “Observably large non-Gaussianity can be obtained by breaking the slow-roll conditions during inflation [14], using extended kinetic terms [15–25], see also the reviews [26, 27], or going beyond models of single-field inflation [11, 28–34] It is natural to consider multiple scalar field since they ar”