Scale-dependent non-Gaussianity probes inflationary physics

By C. Byrnes, Mischa Gerstenlauer, Sami Nurmi, G. Tasinato, D. Wands. 2010

137 citations recorded by the source corpus.

We calculate the scale dependence of the bispectrum and trispectrum in (quasi) local models of non-Gaussian primordial density perturbations, and characterize this scale dependence in terms of new observable parameters. They can help to discriminate between models of inflation, since they are sensitive to properties of the inflationary physics that are not probed by the standard observables. We find consistency relations between these parameters in certain classes of models. We apply our results to a scenario of modulated reheating, showing that the scale dependence of non-Gaussianity can be significant. We also discuss the scale dependence of the bispectrum and trispectrum, in cases where one varies the shape as well as the overall scale of the figure under consideration. We conclude providing a formulation of the curvature perturbation in real space, which generalises the standard local form by dropping the assumption that fNL and gNL are constants.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/707741ff16ef57ba2f6ffe83b3f4db141a83ec4a

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. A. Banday
2. H. Eriksen
3. F. Hansen
4. P. Lilje
5. E. Pajer
6. G. Efstathiou
7. M. Liguori
8. Xingang Chen

In Nuclear and High Energy Physics

1. A. Banday
2. H. Eriksen
3. E. di Valentino
4. P. Lilje
5. F. Hansen
6. Xingang Chen
7. J. Fergusson
8. G. Efstathiou

Citations in the corpus

• Planck 2018 results. IX. Constraints on primordial non-Gaussianity (2019, methodology): “…with canonical kinetic terms, that their correlators are Gaussian at horizon crossing, and using the slowroll approximation and the δN formalism, Byrnes et al. (2010a) found a quite general expression for the power spectrum of the primordial potential perturbation: PΦ(k) = 2π2 k3 PΦ(k) = 2π2…”
• Building a boostless bootstrap for the bispectrum (2020, background): “[45, 46, 47, 48, 49, 50, 51]), with some exceptions such as for example resonant non-Gaussianity [52, 53, 54, 55, 56, 57, 58, 59].”