Primordial black hole constraints on non-gaussian inflation models

We determine the abundance of primordial black holes (PBHs) formed in the context of non-gaussian models with primordial density perturbations. We consider models with a renormalized $χ^2$ probability distribution function parametrized by the number, $ν$, of degrees of freedom. We show that if $ν$ is not too large then the PBH abundance will be altered by several orders of magnitude with respect to the standard gaussian result obtained in the $ν\to \infty$ limit. We also study the dependence of the spectral index constraints on the nature of the cosmological perturbations for a power-law primordial power spectrum.

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