Weak initial clustering of primordial black holes reduces the PBH fraction needed to explain LIGO-Virgo-KAGRA mergers in the two-body channel, while strong clustering suppresses the rate via three-body formation.
On the merger rate of primordial black holes: effects of nearest neighbours distribution and clustering
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abstract
One of the seemingly strongest constraints on the fraction of dark matter in the form of primordial black holes (PBH) of ${\cal O}$(10)$\,M_\odot$ relies on the merger rate inferred from the binary BH merger events detected by LIGO/Virgo. The robustness of these bounds depends however on the accuracy with which the formation of PBH binaries in the early Universe can be described. We revisit the standard estimate of the merger rate, focusing on a couple of key ingredients: the spatial distribution of nearest neighbours and the initial clustering of PBHs associated to a given primordial power spectrum. Overall, we confirm the robustness of the results presented in the literature in the case of a narrow mass function (which constrain the PBH fraction of dark matter to be $f_{\rm PBH}\lesssim 0.001-0.01$). The initial clustering of PBHs might have an effect tightening the current constraint, but only for very broad mass functions, corresponding to wide bumps in the primordial power spectra extending at least over a couple of decades in $k$-space.
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Merger rate of initially clustered primordial black holes for the two-body channel
Weak initial clustering of primordial black holes reduces the PBH fraction needed to explain LIGO-Virgo-KAGRA mergers in the two-body channel, while strong clustering suppresses the rate via three-body formation.
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Hunting Dark Matter with the Einstein Telescope
Clustered primordial black holes may constitute all dark matter and produce a flat stochastic gravitational wave background detectable by the Einstein Telescope.
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Primordial Black Holes as Dark Matter: Recent Developments
Primordial black holes in specific mass ranges could account for some or all dark matter while resolving structure-formation and seed problems in standard cosmology.