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Constraints on the density perturbation spectrum from primordial black holes
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abstract
We re-examine the constraints on the density perturbation spectrum, including its spectral index $n$, from the production of primordial black holes. The standard cosmology, where the Universe is radiation dominated from the end of inflation up until the recent past, was studied by Carr, Gilbert and Lidsey; we correct two errors in their derivation and find a significantly stronger constraint than they did, $n \lesssim 1.25$ rather than their 1.5. We then consider an alternative cosmology in which a second period of inflation, known as thermal inflation and designed to solve additional relic over-density problems, occurs at a lower energy scale than the main inflationary period. In that case, the constraint weakens to $n \lesssim 1.3$, and thermal inflation also leads to a `missing mass' range, $10^{18} g \lesssim M \lesssim 10^{26} g$, in which primordial black holes cannot form. Finally, we discuss the effect of allowing for the expected non-gaussianity in the density perturbations predicted by Bullock and Primack, which can weaken the constraints further by up to 0.05.
Forward citations
Cited by 6 Pith papers
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Primordial Black Holes from Vector-Induced Curvature Perturbations Sourced by Primordial Magnetic Fields
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Fine-tuning in mixed Dark Matter models with Primordial Black Hole relics
In mixed dark matter models combining Planck-mass black hole relics, Hawking-evaporated particles, and a WIMP, freeze-in, or axion component, the total abundance's fine-tuning is dominated by the primordial power spec...
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The Gravitational Spectral Radio Forest: A Signature of Primordial Black Holes
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Constraints on Primordial Black Holes
Updated compilation shows PBHs are tightly constrained across 55 orders of magnitude in mass, ruling out dominant dark matter contributions except in narrow windows, with many limits carrying observational uncertainties.
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Primordial Black Holes: A Review of Formation and Evolution
Review of PBH formation via compaction function and relativistic thresholds in FLRW backgrounds, arguing that memory burden and curvature corrections halt evaporation to leave Planck-scale relics.
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