Scalar spectral index in the presence of Primordial Black Holes

TL;DR

This paper investigates how primordial black holes formed from inflationary inhomogeneities can constrain the scalar spectral index, using observational data to limit the small-scale perturbations and their impact on early universe reheating.

Contribution

It introduces a method to constrain the scalar spectral index by analyzing PBH formation and evaporation, linking small-scale perturbations to cosmological observations.

Findings

Upper bounds on n_s: 1.309 for ζ_th=0.7 and 1.334 for ζ_th=1.2

PBH mass range constrained to 10^9-10^11 g

Estimated density fraction contributing to PBH formation

Abstract

We study the possibility of reheating the universe in its early stages through the evaporation of Primordial Black Holes (PBHs) that are formed due to the collapse of the inhomogeneities that were generated during inflation. By using the current results of the baryon-photon ratio obtained from BBN and CMB observations, we impose constraints on the spectral index of perturbations on those small scales that cannot be estimated through CMB anisotropy and CMB distortions. The masses of the PBHs constrained in this study lie in the range of $10^{9}$ and $10^{11}$g, which corresponds to those PBHs whose maximal evaporation took place during the redshifts $10^{6} < z < 10^{9}$. It is shown that the upper bound on the scalar spectral index, $ n_{s}$ can be constrained for a given threshold value, $ \zeta _{\rm th}$, of the curvature perturbations for PBHs formation. Using Planck results for cosmological parameters we obtained $n_{s} < 1.309 $ for $ \zeta _{\rm th} =0.7 $ and $ n_{s} < 1.334 $ for $ \zeta _{\rm th} = 1.2 $ respectively. The density fraction that has contributed to the formation of Primordial Black Holes has also been estimated.