arXiv : Detecting the Stochastic Gravitational Wave Background from Primordial Black Hole Formation

Clesse, Sebastien; García-Bellido, Juan; Orani, Stefano

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Preprint
Report number	arXiv:1812.11011 ; IFT--UAM/CSIC--17--119 ; CERN--TH--2017--259 ; CERN-TH-2017-259
Title	Detecting the Stochastic Gravitational Wave Background from Primordial Black Hole Formation
Author(s)	Clesse, Sebastien (Louvain U.) ; García-Bellido, Juan (CSIC, Madrid ; CERN) ; Orani, Stefano (Louvain U.)
Publication	2018
Imprint	2018-12-28
Number of pages	20
Note	* Temporary entry * * Temporary entry * 20 pages, 5 figures, comments welcome
Subject category	hep-th ; Particle Physics - Theory ; gr-qc ; General Relativity and Cosmology ; astro-ph.CO ; Astrophysics and Astronomy
Abstract	Primordial Black Holes (PBH) from peaks in the curvature power spectrum could constitute today an important fraction of the Dark Matter in the Universe. At horizon reentry, during the radiation era, order one fluctuations collapse gravitationally to form black holes and, at the same time, generate a stochastic background of gravitational waves coming from second order anisotropic stresses in matter. We study the amplitude and shape of this background for several phenomenological models of the curvature power spectrum that can be embedded in waterfall hybrid inflation, axion, domain wall, and boosts of PBH formation at the QCD transition. For a broad peak or a nearly scale invariant spectrum, this stochastic background is generically enhanced by about one order of magnitude, compared to a sharp feature. As a result, stellar-mass PBH from Gaussian fluctuations with a wide mass distribution are already in strong tension with the limits from Pulsar Timing Arrays, if they constitute a non negligible fraction of the Dark Matter. But this result is mitigated by the uncertainties on the curvature threshold leading to PBH formation. LISA will have the sensitivity to detect or rule out light PBH down to $10^{-14} M_{\odot}$. Upcoming runs of LIGO/Virgo and future interferometers such as the Einstein Telescope will increase the frequency lever arm to constrain PBH from the QCD transition. Ultimately, the future SKA Pulsar Timing Arrays could probe the existence of even a single stellar-mass PBH in our Observable Universe.
Other source	Inspire
Copyright/License	preprint: (License: arXiv nonexclusive-distrib 1.0)

$Spectrum of primordial curvature perturbations at the end of inflation $\mathcal{P}_{\zeta}$ as a function of $k$. Top: For the Gaussian model (\ref{eq:phi}), with $k_{\rm p} = 2 \times 10^6 {\rm Mpc}^{-1}$, $\sigma_{\rm p } = 3$ and $\mathcal P_{\rm p} = 0.025 $. Center-top: For the sharp peak model, assuming a thin Gaussian with $\sigma_{\rm p} = 0.1$ and $\mathcal P _{\rm p} = 0.0298 $. Center-bottom: For the broken power-law model (\ref{eq:pl}), with $m=3$, $n=0.5$ and $\mathcal{P}_p=0.0275$. Bottom: for the nearly-flat model with boosted formation at QCD, with $n_{\rm p} = 0.96 $, $k_{\rm min} = 10^{3} {\rm Mpc}^{-1}$ and $P_{p} = 0.0205 $. All models lead to $f_{\rm PBH}^{\rm tot} = 1$ today, i.e. PBH account for all the Dark Matter. The red vertical lines illustrate the window of modes considered for the evaluation of gravitational waves from PBH formation.$ $Spectrum of primordial curvature perturbations at the end of inflation $\mathcal{P}_{\zeta}$ as a function of $k$. Top: For the Gaussian model (\ref{eq:phi}), with $k_{\rm p} = 2 \times 10^6 {\rm Mpc}^{-1}$, $\sigma_{\rm p } = 3$ and $\mathcal P_{\rm p} = 0.025 $. Center-top: For the sharp peak model, assuming a thin Gaussian with $\sigma_{\rm p} = 0.1$ and $\mathcal P _{\rm p} = 0.0298 $. Center-bottom: For the broken power-law model (\ref{eq:pl}), with $m=3$, $n=0.5$ and $\mathcal{P}_p=0.0275$. Bottom: for the nearly-flat model with boosted formation at QCD, with $n_{\rm p} = 0.96 $, $k_{\rm min} = 10^{3} {\rm Mpc}^{-1}$ and $P_{p} = 0.0205 $. All models lead to $f_{\rm PBH}^{\rm tot} = 1$ today, i.e. PBH account for all the Dark Matter. The red vertical lines illustrate the window of modes considered for the evaluation of gravitational waves from PBH formation.$ $PBH mass spectrum, $f_{\rm PBH} \equiv {\rm d } \rho_{\rm PBH} / {\rm d} \ln \mPBH$ vs. the PBH mass $\mPBH$ in solar mass units, for the considered models (blue: Gaussian peak, green: sharp peak, red: broken power-law, orange: nearly-flat spectrum with QCD boost) and parameters as in Fig.~\ref{fig:specs}. All models lead to $f_{\rm PBH}^{\rm tot} = 1$, i.e. PBH make all the Dark Matter.$ Show more plots

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記錄創建於2019-01-02，最後更新在2021-05-20

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