2025/12/03 by Chudaykin, Anton, Ivanov, Mikhail M., Philcox, Oliver H. E.
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #High Energy Physics - Phenomenology (hep-ph) #High Energy Physics - Theory (hep-th)
paper · doi:10.48550/arxiv.2512.04266
openalex publication_date 2025/12/03 · openalex created_date 2025/12/06 · openalex updated_date 2026/07/28
Models of cosmic inflation generically predict a weak but potentially detectable amount of primordial non-Gaussianity (PNG), which can be used to obtain insights into the degrees of freedom during inflation and their interactions. The simplest types of PNG are the local and non-local (equilateral and orthogonal) shapes of the primordial three-point correlators, which are predicted by models with multiple light fields and derivative interactions in single-field inflation, respectively. In this paper we place constraints on local, equilateral, and orthogonal non-Gaussianities using the power spectrum and bispectrum extracted from first public release of the Dark Energy Spectroscopic Instrument (DESI). Our analysis makes use of higher-order clustering information through a consistent effective field theory (EFT) model for both the power spectrum and bispectrum at one-loop order. Using robust scale cuts where the EFT description is valid, we find the following constraints on PNG amplitudes: f\rm loc\rm NL=-0.1± 7.4, f\rm equil\rm NL=719± 390, f\rm orth\rm NL=-200± 100 (at 68% CL). Non-local PNG constraints can be further improved by combining high-redshift DESI with legacy BOSS data and using simulation-based priors on bias parameters, yielding the strongest large-scale structure constraints to date f\rm equil\rm NL=200± 230, f\rm orth\rm NL=-24± 86. Our constraint on f\rm loc\rm NL is competitive with the cosmic microwave background (CMB) limit; the combination gives f\rm loc\rm NL=-0.0± 4.1, 18% stronger than the CMB only result, which represents the strongest bound on multi-field inflation yet obtained.