Primordial black holes from a curvaton scenario with strongly non-Gaussian perturbations
A Gow, T Miranda, S Nurmi - Journal of Cosmology and …, 2023 - iopscience.iop.org
A Gow, T Miranda, S Nurmi
Journal of Cosmology and Astroparticle Physics, 2023•iopscience.iop.orgWe investigate the production of primordial black holes (PBHs) in a mixed inflaton-curvaton
scenario with a quadratic curvaton potential, assuming the curvaton is in de Sitter
equilibrium during inflation with< χ>= 0. In this setup, the curvature perturbation sourced by
the curvaton is strongly non-Gaussian, containing no leading Gaussian term. We show that
for m 2/H 2≳ 0.3, the curvaton contribution to the spectrum of primordial perturbations on
CMB scales can be kept negligible but on small scales the curvaton can source PBHs. In …
scenario with a quadratic curvaton potential, assuming the curvaton is in de Sitter
equilibrium during inflation with< χ>= 0. In this setup, the curvature perturbation sourced by
the curvaton is strongly non-Gaussian, containing no leading Gaussian term. We show that
for m 2/H 2≳ 0.3, the curvaton contribution to the spectrum of primordial perturbations on
CMB scales can be kept negligible but on small scales the curvaton can source PBHs. In …
Abstract
We investigate the production of primordial black holes (PBHs) in a mixed inflaton-curvaton scenario with a quadratic curvaton potential, assuming the curvaton is in de Sitter equilibrium during inflation with< χ>= 0. In this setup, the curvature perturbation sourced by the curvaton is strongly non-Gaussian, containing no leading Gaussian term. We show that for m 2/H 2≳ 0.3, the curvaton contribution to the spectrum of primordial perturbations on CMB scales can be kept negligible but on small scales the curvaton can source PBHs. In particular, PBHs in the asteroid mass range 10-16 M⊙≲ M≲ 10-10 M⊙ with an abundance reaching F PBH= 1 can be produced when the inflationary Hubble scale H≳ 10 12 GeV and the curvaton decay occurs in the window from slightly before the electroweak transition to around the QCD transition.
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