The effect of outflows on CMB bounds from Primordial Black Hole accretion

Article
Report number	arXiv:2210.14934 ; ULB-TH/22-14 ; UTWI-11-2022
Title	The effect of outflows on CMB bounds from Primordial Black Hole accretion
Related title	The effect of outflows on CMB bounds from Primordial Black Hole accretion
Author(s)	Piga, Lorenzo (Parma U. ; INFN, Parma) ; Lucca, Matteo (Brussels U.) ; Bellomo, Nicola (Texas U., TCC) ; Bosch-Ramon, Valentì (ICC, Barcelona U.) ; Matarrese, Sabino (U. Padua, Dept. Phys. Astron. ; INFN, Padua ; Padua Observ. ; GSSI, Aquila) ; Raccanelli, Alvise (U. Padua, Dept. Phys. Astron. ; INFN, Padua ; Padua Observ. ; CERN) ; Verde, Licia (ICC, Barcelona U. ; ICREA, Barcelona)
Publication	2022-12-12
Imprint	2022-10-26
Number of pages	36
Note	34 pages, 8 figures
In:	JCAP 2212 (2022) 016
DOI	10.1088/1475-7516/2022/12/016
Subject category	astro-ph.CO ; astro-ph.HE ; gr-qc ; Astrophysics and Astronomy
Abstract	Should Primordial Black Holes (PBHs) exist in nature, they would inevitably accrete baryonic matter in their vicinity. In turn, the consequent emission of high-energy radiation could affect the thermal history of the universe to an extent that can be probed with a number of cosmological observables such as the Cosmic Microwave Background (CMB) anisotropies. However, our understanding of the accretion and radiation emission processes in the context of PBHs is still in its infancy, and very large theoretical uncertainties affect the resulting constraints on the PBH abundance. Building on state-of-the-art literature, in this work we take a step towards the development of a more realistic picture of PBH accretion by accounting for the contribution of outflows. Specifically, we derive CMB-driven constraints on the PBH abundance for various accretion geometries, ionization models and mass distributions in absence and in presence of mechanical feedback and non-thermal emissions due to the outflows. As a result, we show that the presence of such outflows introduces an additional layer of uncertainty that needs to be taken into account when quoting cosmological constraints on the PBH abundance, with important consequences in particular in the LIGO-Virgo-KAGRA observational window.
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0) publication: © 2022-2024 IOP Publishing Ltd and Sissa Medialab

$Graphical illustration of the impact that the three possible choices for the computation of the relative velocity between PBH and surrounding matter have on the final luminosity of the system, for both the collisional (left) and photo-ionization (right) models. As term of reference, we compare the average radiation luminosity $\langle L_{\rm rad} \rangle$ to the Eddington luminosity~$L_\mathrm{edd}$.$ $Graphical illustration of the impact that the three possible choices for the computation of the relative velocity between PBH and surrounding matter have on the final luminosity of the system, for both the collisional (left) and photo-ionization (right) models. As term of reference, we compare the average radiation luminosity $\langle L_{\rm rad} \rangle$ to the Eddington luminosity~$L_\mathrm{edd}$.$ $Graphical illustration of the dependence of the emission efficiency $\epsilon$ on the geometry of the accretion (spherical on the left, disk on the right) as well as on the ionization mechanism (photoionization as solid lines, collisional ionization as dashed lines) for different choices of the PBH mass. In all cases we assume $f_{\rm PBH}=1$. The horizontal dashed-dotted lines represent the benchmark outflow efficiencies $\epsilon_{\rm non-th}$ discussed in section \ref{subsec: imp_lum}.$ Show more plots

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