In single-field PBH inflation models, a power-spectrum dip appears precisely when the inflaton velocity does not flip sign, and the peak amplitude scales as the inverse square of the dip amplitude.
Primordial Black Holes from No-Scale Supergravity
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We calculate the primordial black hole abundance in the context of a Wess-Zumino type no-scale supergravity model. We modify the K\"ahler potential, by adding an extra exponential term. Using just one parameter in the context of this model, we are able to satisfy the Planck cosmological constraints for the spectral index $n_s$, the tensor-to-scalar ratio $r$, and to produce up to $\sim 20\%$ of the dark matter of the Universe in the form of primordial black holes.
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How deep is the dip and how tall are the wiggles in inflationary power spectra?
In single-field PBH inflation models, a power-spectrum dip appears precisely when the inflaton velocity does not flip sign, and the peak amplitude scales as the inverse square of the dip amplitude.