Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component

TL;DR

This paper revisits the gravitational wave background from primordial black hole reheating, showing that including realistic mass spread suppresses the dominant Poltergeist signal, making scalar-induced waves more relevant.

Contribution

It introduces a detailed analysis of the minimal mass spread effect on gravitational wave signals from PBH reheating, revealing new viable parameter space.

Findings

Mass spread smooths reheating, suppressing Poltergeist GW background.

Scalar-induced GW signals dominate in certain early matter scenarios.

Previously excluded PBH parameter regions are now viable under new constraints.

Abstract

The reheating of the universe by the evaporation of light primordial black holes (PBHs) can leave a stochastic gravitational-wave (GW) background in the early Universe. In the monochromatic limit, their simultaneous evaporation produces an abrupt matter-to-radiation transition, triggering the so-called Poltergeist GW signal, usually predicted to be dominant and observable. We revisit this result by including the irreducible mass spread implied by gravitational collapse in General Relativity, whose infrared tail scales as $d f_{\rm PBH}/d\ln M_{\rm PBH}\propto M_{\rm PBH}^{3.78}$. We show that this minimal width smooths reheating enough to suppress the Poltergeist background by orders of magnitude, down to the level of the scalar-induced GW signal produced during a generic early matter era, such as one driven by the decay of a heavy relic. We provide a complete decomposition of the scalar-induced spectrum into eight production channels and find that none, except the one from PBH formation, reaches either the $\Delta N_{\rm eff}$ bound or the projected sensitivity of future GW observatories. This reopens regions of ultra-light PBH parameter space previously thought to be excluded by these constraints.