Why Must Primordial Non-Gaussianity Be Very Small?

Abstract

One-loop correction to the power spectrum in generic single-field inflation is calculated by using standard perturbation theory. Because of the enhancement inversely proportional to the observed red tilt of the spectral index of curvature perturbation, the correction turns out to be much larger than previously anticipated. As a result, the primordial non-Gaussianity must be much smaller than the current observational bound in order to warrant the validity of cosmological perturbation theory.

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Cited by in corpus (14)

• Inflation and Primordial Black Holes
• Implications for the non-Gaussianity of curvature perturbation from pulsar timing arrays
• Questions on calculation of primordial power spectrum with large spikes: the resonance model case
• Constraining Primordial Black Hole Formation from Single-Field Inflation
• One-loop correction to the enhanced curvature perturbation with local-type non-Gaussianity for the formation of primordial black holes
• Observational imprints of enhanced scalar power on small scales in ultra slow roll inflation and associated non-Gaussianities
• Loop contributions to the scalar power spectrum due to quartic order action in ultra slow roll inflation
• Growth of curvature perturbations for PBH formation \& detectable GWs in non-minimal curvaton scenario revisited
• Comparing sharp and smooth transitions of the second slow-roll parameter in single-field inflation
• Primordial black holes and third order scalar induced gravitational waves
• Perturbative region on non-Gaussian parameter space in single-field inflation
• Inflationary cross-correlations of a non-minimal spectator and their soft limits
• Revisiting the Chern-Simons interaction during inflation with a non-canonical pseudo-scalar
• A Tail of Eternal Inflation