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 $\chi^2$ probability distribution function parametrized by the number, $\nu$, of degrees of freedom. We show that if $\nu$ 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 $\nu \to \infty$ 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.