Primordial black hole formation and abundance: contribution from the non-linear relation between the density and curvature perturbation
By S. Young, I. Musco, C. Byrnes. Journal of Cosmology and Astroparticle Physics, 2019
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The formation and abundance of primordial black holes (PBHs) arising from the curvature perturbation ζ is studied. The non-linear relation between ζ and the density contrast δ means that, even when ζ has an exactly Gaussian distribution, significant non-Gaussianities affecting PBH formation must be considered. Numerical simulations are used to investigate the critical value and the mass of PBHs which form, and peaks theory is used to calculate the mass fraction of the universe collapsing to form PBHs at the time of formation. A formalism to calculate the total present day PBH abundance and mass function is also derived. It is found that the abundance of PBHs is very sensitive to the non-linear effects, and that the power spectrum 𝒫ζ must be a factor of 𝒪 (2) larger to produce the same number of PBHs as if using the linear relation between ζ and δ (where the exact value depends on the critical value for a region to collapse and form a PBH). This also means that the derived constraints on the small-scale power spectrum from constraints on the abundance of PBHs are weaker by the same factor.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/ad1f0e54915e4453efb3260b2dddf7803c7c6e92
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Citations in the corpus
- The exponential tail of inflationary fluctuations: consequences for primordial black holes (2019, background): “Non-Gaussianities may therefore play a crucial role in determining the abundance of PBHs [37–50] and, in this work, we provide a generic, non-perturbative framework to derive the tails of the PDFs of curvature perturbations.”
- Primordial black holes and gravitational waves from parametric amplification of curvature perturbations (2019, methodology): “ns and the anisotropic stress, the perturbed metric reads, ds2 = a2(˝) ˆ (1 + 2) d˝2 + (1 2) ij+ 1 2 h ij dxidxj ˙ ; (4.1) 3Non-Gaussianity is generated in this kind of models [73{75]. In Refs. [57,76], it is found that nonGaussianity can aect the PBH abundance. However, using the method of [77],”