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Detection prospects for the GW background of Galactic (sub)solar mass primordial black holes
Cosmology and Nongalactic Astrophysics · Submitted 6 Oct 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim While this signal remains below the LISA detection threshold for viable $f_\text{pbh}\lesssim 0.01$, future GW observatories such as DECIGO and BBO could detect it if $0.01\lesssim M_{\rm pbh} \lesssim 0.1 M_\odot$.
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The abstract, sentence by sentence
In multi-component dark matter models, a fraction $f_\text{pbh}$ of the dark matter could be in the form of primordial black holes (PBHs) with (sub)solar masses. Some would have formed binaries that presently trace the Milky Way halo of particle dark matter. We explore the gravitational wave (GW) signal produced by such a hypothetical population of Galactic PBH binaries and assess its detectability by the LISA experiment. For this purpose, we model the formation and evolution of early-type PBH binaries accounting for GW hardening and binary disruption in the Milky Way. Our analysis reveals that the present-day Galactic population of PBH binaries is characterized by very high orbital eccentricities $|1-e|\ll 1$. For a PBH mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$, this yields a GW background that peaks in the millihertz frequency range where the LISA instrumental noise is minimum. While this signal remains below the LISA detection threshold for viable $f_\text{pbh}\lesssim 0.01$, future GW observatories such as DECIGO and BBO could detect it if $0.01\lesssim M_{\rm pbh} \lesssim 0.1 M_\odot$. Furthermore, we anticipate that, after 5 years of observations, LISA should be able to detect $\mathcal{O}(100)$ (resp. $\mathcal{O}(1)$) loud Galactic PBH binaries of mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$ with a SNR $\geq 5$ if $f_{\rm pbh}=0.01$ (resp. $f_{\rm pbh}=0.001$). Nonlinear effects not considered here such as mass accretion and dynamical capture could alter these predictions.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In multi-component dark matter models, a fraction $f_\text{pbh}$ of the dark matter could be in the form of primordial black holes (PBHs) with (sub)solar masses. | background 1.00 | 0.05 | 0.03 | hedged possibility 1.00 |
| s1 | Some would have formed binaries that presently trace the Milky Way halo of particle dark matter. | background 0.99 | 0.06 | 0.02 | hedged possibility 0.71 |
| s2 | We explore the gravitational wave (GW) signal produced by such a hypothetical population of Galactic PBH binaries and assess its detectability by the LISA experiment. | contribution 0.99 | 0.77 | 0.04 | asserted 0.70 |
| s3 | For this purpose, we model the formation and evolution of early-type PBH binaries accounting for GW hardening and binary disruption in the Milky Way. | method 1.00 | 0.86 | 0.02 | asserted 0.94 |
| s4 | Our analysis reveals that the present-day Galactic population of PBH binaries is characterized by very high orbital eccentricities $|1-e|\ll 1$. | result 1.00 | 0.93 | 0.13 | asserted 1.00 |
| s5 | For a PBH mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$, this yields a GW background that peaks in the millihertz frequency range where the LISA instrumental noise is minimum. | result 0.89 | 0.83 | 0.15 | asserted 0.98 |
| s6 | While this signal remains below the LISA detection threshold for viable $f_\text{pbh}\lesssim 0.01$, future GW observatories such as DECIGO and BBO could detect it if $0.01\lesssim M_{\rm pbh} \lesssim 0.1 M_\odot$. | result 0.82 | 0.81 | 0.36 | hedged possibility 0.79 |
| s7 | Furthermore, we anticipate that, after 5 years of observations, LISA should be able to detect $\mathcal{O}(100)$ (resp. $\mathcal{O}(1)$) loud Galactic PBH binaries of mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$ with a SNR $\geq 5$ if $f_{\rm pbh}=0.01$ (resp. $f_{\rm pbh}=0.001$). | result 0.98 | 0.80 | 0.23 | hedged possibility 0.84 |
| s8 | Nonlinear effects not considered here such as mass accretion and dynamical capture could alter these predictions. | limitation 1.00 | 0.15 | 0.02 | hedged possibility 1.00 |
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The paper
Original abstract
In multi-component dark matter models, a fraction $f_\text{pbh}$ of the dark matter could be in the form of primordial black holes (PBHs) with (sub)solar masses. Some would have formed binaries that presently trace the Milky Way halo of particle dark matter. We explore the gravitational wave (GW) signal produced by such a hypothetical population of Galactic PBH binaries and assess its detectability by the LISA experiment. For this purpose, we model the formation and evolution of early-type PBH binaries accounting for GW hardening and binary disruption in the Milky Way. Our analysis reveals that the present-day Galactic population of PBH binaries is characterized by very high orbital eccentricities $|1-e|\ll 1$. For a PBH mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$, this yields a GW background that peaks in the millihertz frequency range where the LISA instrumental noise is minimum. While this signal remains below the LISA detection threshold for viable $f_\text{pbh}\lesssim 0.01$, future GW observatories such as DECIGO and BBO could detect it if $0.01\lesssim M_{\rm pbh} \lesssim 0.1 M_\odot$. Furthermore, we anticipate that, after 5 years of observations, LISA should be able to detect $\mathcal{O}(100)$ (resp. $\mathcal{O}(1)$) loud Galactic PBH binaries of mass $M_{\rm pbh} \sim 0.1 - 1 M_\odot$ with a SNR $\geq 5$ if $f_{\rm pbh}=0.01$ (resp. $f_{\rm pbh}=0.001$). Nonlinear effects not considered here such as mass accretion and dynamical capture could alter these predictions.
Human review
References
How the literature uses it
3 arXiv papers cite this in 7 sentences
Papers citing it · 6 sentences without a confident label
Uses its method or tool 1 paper
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Here we follow the approach in Refs. [ref] (see also [ref] ).
Gravitational Waves From Dark Binaries With Finite-Range Dark Forces · Binary distribution with a finite mediator mass · 0.86
What it cites · 100 sentences without a confident label
Uses the method or tool of 15 papers
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For the range of $f$ and $m$ considered here, typical values of $x_i$ are much lower than the $s-$comoving Hubble radius $ℋ_eq^-1≃6·10^9$, so that we can compute the evolution of the distance to the nearest neighbor using a Newtonian approximation, as in [ref] .
The merger rate of primordial-black-hole binaries · Formation of PBH binaries · 0.86
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The SNR is computed as follows [ref] : [equation] where we have defined [equation] Note that the parameter vector $$ does not include the inclination $$, which is averaged out from this expression.
The construction and use of LISA sensitivity curves · Confusion noise from unresolved Galactic DWDs · 0.98
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The SNR is computed as follows [ref] : [equation] where we have defined [equation] Note that the parameter vector $$ does not include the inclination $$, which is averaged out from this expression.
2305.09372 · Confusion noise from unresolved Galactic DWDs · 0.98
Uses data or values from 18 papers
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The number $N_0$ of PBH binaries expected to reside in the MW halo is given by [equation] assuming a MW DM mass of $M_DM= 2×10^12$ [ref] and a monochromatic PBH mass spectrum with $=m$.
The effects of dynamical substructure on Milky Way mass estimates from the high velocity tail of the local stellar halo · Introduction · 1.00
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The number $N_0$ of PBH binaries expected to reside in the MW halo is given by [equation] assuming a MW DM mass of $M_DM= 2×10^12$ [ref] and a monochromatic PBH mass spectrum with $=m$.
The mass of the Milky Way and M31 using the method of least action · Introduction · 1.00
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Following [ref] , we take $σ_eq = 0.005$ for our numerical estimates[In many scenarios PBH formation is accompanied by an enhancement of the primordial power at small scales [ref] .
Density Perturbations and Black Hole Formation in Hybrid Inflation · Time evolution of the reduced angular momentum · 0.88
Compares with 9 papers
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This agrees with the predictions of [ref] (see their Fig. 4).
The merger rate of primordial-black-hole binaries · Hardening through GW emission · 0.96
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The confusion noise of unresolved DWD GW sources represented by the dashed blue curve is consistent with other estimates from the literature [ref] .
The Gravitational Wave Background from Cosmological Compact Binaries · Confusion noise from unresolved Galactic DWDs · 0.98
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The confusion noise of unresolved DWD GW sources represented by the dashed blue curve is consistent with other estimates from the literature [ref] .
Gravitational-wave emission from compact Galactic binaries · Confusion noise from unresolved Galactic DWDs · 0.98
Cites as support 4 papers
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Furthermore, since PBH models in the (sub)solar mass range with fractions $f>0.01$ are severely constrained by microlensing events [ref] , we shall hereafter present results for $f≲0.01$ only.
No massive black holes in the Milky Way halo · Evolution of Galactic PBH binaries · 0.98
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A refined model for $j(t)$ in RD would not have changed our results significantly, since angular momentum accretion is small in the RD era, and PBH binaries forming before equality have high eccentricities $|1-e_*|≲1$ [ref] .
The merger rate of primordial-black-hole binaries · Time evolution of the reduced angular momentum · 0.99
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A refined model for $j(t)$ in RD would not have changed our results significantly, since angular momentum accretion is small in the RD era, and PBH binaries forming before equality have high eccentricities $|1-e_*|≲1$ [ref] .
Formation and Evolution of Primordial Black Hole Binaries in the Early Universe · Time evolution of the reduced angular momentum · 0.99
Cites as background 20 papers
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Close pairs of PBHs can form binaries in the early Universe and emit GWs at frequencies dependent on their masses (for reviews, see [ref] ).
Probing Primordial Black Hole Scenarios with Terrestrial Gravitational Wave Detectors · Introduction · 0.99
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Close pairs of PBHs can form binaries in the early Universe and emit GWs at frequencies dependent on their masses (for reviews, see [ref] ).
Primordial black holes and their gravitational-wave signatures · Introduction · 0.99
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Close pairs of PBHs can form binaries in the early Universe and emit GWs at frequencies dependent on their masses (for reviews, see [ref] ).
Lectures on Gravitational Wave Signatures of Primordial Black Holes · Introduction · 0.99
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