Primordial Black Hole Formation from Power Spectrum with Finite-width

Abstract

Primordial black holes (PBHs) can form from gravitational collapse of large overdensities in the early Universe, giving rise to rich phenomena in astrophysics and cosmology. We develop a novel, general, and systematic method based on theory of density contrast peaks to calculate the abundance of PBHs for a broad power spectrum of curvature perturbations with Gaussian statistics. We introduce a window function to account for the relevant perturbation scales associated with PBHs of different masses, along with a filter function that removes unphysical contributions from super-horizon-scale overdensities. While some uncertainties remain due to the limited understanding of the nonlinear collapse process, our approach substantially reduces the discrepancy previously observed between peaks theory and the Press-Schechter formalism.

61 pages, 30 figures

References in corpus (2)

• Curbing PBHs with PTAs
• Numerical simulation of type II primordial black hole formation

Cited by in corpus (7)

• Fundamental Physics and Cosmology with TianQin
• Threshold for PBH formation in the type-II region and its analytical estimation
• Beware of the running $n_s$ when producing heavy primordial black holes
• Inflationary relics from an Ultra-Slow-Roll plateau
• Numerical simulations of primordial black hole formation via delayed first-order phase transitions
• Primordial black hole formation in k-inflation models
• Effect of stochastic kicks on primordial black hole abundance and mass via the compaction function