Primordial trispectrum from inflation

By C. Byrnes, Misao Sasaki, D. Wands. 2006

229 citations recorded by the source corpus.

We use the delta N-formalism to describe the leading order contributions tothe primordial power spectrum, bispectrum and trispectrum in multiple-fieldmodels of inflation at leading order in a perturbative expansion. In slow-rollmodels where the initial field fluctuations at Hubble-exit are nearly Gaussian,any detectable non-Gaussianity is expected to come from super-Hubble evolution.We show that the contribution to the primordial trispectrum can be described bytwo non-linearity parameters, tau_{NL} and g_{NL}, which are dependent upon thesecond and third derivatives of the local expansion with respect to the fieldvalues during inflation.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/37c4a1115a59385183aec628c823749adbfde82f

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. D. Baumann
2. M. Zaldarriaga
3. E. Komatsu
4. C. Byrnes
5. L. Senatore
6. Xingang Chen
7. D. Green
8. D. Seery

In Nuclear and High Energy Physics

1. D. Baumann
2. C. Byrnes
3. Kiwoon Choi
4. D. Seery
5. E. Komatsu
6. F. Vernizzi
7. Xingang Chen
8. D. Green

Citations in the corpus

• Large-scale bias and efficient generation of initial conditions for nonlocal primordial non-Gaussianity (2011, methodology): “Furthermore, using such “average” kernel will in general give an incorrect configuration dependence to the “snake” diagrams of the four-point function that depend on the square of the quadratic kernel (usually characterized by the τNL parameter, see [34]), since the averaging and squaring do not com”
• PRIMORDIAL NON-GAUSSIANITY, SCALE-DEPENDENT BIAS, AND THE BISPECTRUM OF GALAXIES (2009, background): “Recently, a number of groups (e.g., Boubekeur & Lyth 2006; Huang & Shiu 2006; Byrnes et al. 2006; Buchbinder et al. 2008) have shown that the primordial trispectrum can in general be written as TΦ(k1, k2, k3, k4) =6gNL [Pφ(k1)Pφ(k2)Pφ(k3) + (3 cyclic)] + 25 18 τNL × [Pφ(k1)Pφ(k2) {Pφ(k13) +…”
• COrE (Cosmic Origins Explorer) A White Paper (2011, background): “There are also models with a negligible bispectrum and a large trispectrum, including inflation with a parity symmetry [92, 73] and cosmic strings [81].”
• On soft limits of inflationary correlation functions (2012, background): “2) reduce to the familiar (momentum-independent) definitions of fNL [32] and τNL [21].”
• Review of local non-Gaussianity from multi-field inflation (2010, background): “where k13 ≡ |k1 + k3|, and the trispectrum nonlinearity parameters can be calculated using [98, 106, 127]”