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Gravitational wave constraints on extended dark matter structures
Cosmology and Nongalactic Astrophysics · Submitted 30 May 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that LIGO is sensitive to dark objects with radius $O(10-10^3~{\rm km})$ if they make up more than $\sim O(10^{-2}-10^{-3})$ of dark matter.
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The abstract, sentence by sentence
We generalise existing constraints on primordial black holes to dark objects with extended sizes using the aLIGO design sensitivity. We show that LIGO is sensitive to dark objects with radius $O(10-10^3~{\rm km})$ if they make up more than $\sim O(10^{-2}-10^{-3})$ of dark matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We generalise existing constraints on primordial black holes to dark objects with extended sizes using the aLIGO design sensitivity. | contribution 0.96 | 0.88 | 0.09 | asserted 0.95 |
| s1 | We show that LIGO is sensitive to dark objects with radius $O(10-10^3~{\rm km})$ if they make up more than $\sim O(10^{-2}-10^{-3})$ of dark matter. | result 1.00 | 0.91 | 0.83 | asserted 1.00 |
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The paper
Original abstract
We generalise existing constraints on primordial black holes to dark objects with extended sizes using the aLIGO design sensitivity. We show that LIGO is sensitive to dark objects with radius $O(10-10^3~{\rm km})$ if they make up more than $\sim O(10^{-2}-10^{-3})$ of dark matter.
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How the literature uses it
9 arXiv papers cite this in 15 sentences
Papers citing it · 9 sentences without a confident label
Cites it as background 5 papers
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These celestial objects, potentially formed in the early universe, are primarily detectable via their gravitational effects: gravitational lensing (e.g. [ref] ) and gravitational waves (e.g. [ref] ).
Microlensing signatures of extended dark objects using machine learning · Introduction · 0.92
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Recently, gravitational constraints on generic EDOs have been derived from the non-observation of micro-lensing events [ref] , gravitational wave production [ref] , the evaporation of wide binaries [ref] , dynamical heating of dwarf galaxies [ref] , and heating of the CMB due to baryonic accretion [ref] .
Updated constraints on the primordial power spectrum at sub-Mpc scales · Updated EDO limits · 0.88
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Gravitational probes include lensing [ref] , pulsar timing [ref] , accretion [ref] , dynamical friction [ref] , and gravitational waves [ref] .
Constraining axion and compact dark matter with interstellar medium heating · Models of compact DM · 0.88
What it cites · 44 sentences without a confident label
Uses the method or tool of 3 papers
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We can estimate the sensitivity to extended objects using the signal-to-noise ratio $ρ$: [equation] with the value averaged over sky position, inclination, and polarisation $⟨ρ^2 ⟩= 4 ρ^2/25$ [ref] .
Hunting for Dark Particles with Gravitational Waves · Gravitational waves from compact object mergers · 0.92
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Assuming two equal masses $M$ moving with a relative velocity $v$, the cross-section for this process is [ref] [equation] Here we have followed the example of [ref] and neglected three-body encounters, which typically lead to wide binaries which do not merge in a Hubble time [ref] .
Did LIGO detect dark matter? · Merger rate in present-day halos · 0.84
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Assuming two equal masses $M$ moving with a relative velocity $v$, the cross-section for this process is [ref] [equation] Here we have followed the example of [ref] and neglected three-body encounters, which typically lead to wide binaries which do not merge in a Hubble time [ref] .
Runaway Merging of Black Holes: Analytical Constraint on the Timescale · Merger rate in present-day halos · 0.84
Uses data or values from 1 paper
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For the binaries that formed before matter-radiation equality and merged only recently, the rate is calculated in [ref] to be [equation] Here the number $3.4×10^-5$ is the variance of density perturbations of the rest of the dark matter at matter-radiation equality.
The merger rate of primordial-black-hole binaries · Merger rate in the early universe · 0.96
Compares with 2 papers
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The rate derived from this halo mass function [ref] matches our back-of-the-envelope result.] However, one needs to impose a lower limit on the mass of the galaxies because small galaxies can evaporate before creating a merger signal.
Did LIGO detect dark matter? · Merger rate in present-day halos · 0.81
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For celestial objects with small radii, the sensitivity to compact object mergers largely compliments the constraints found from microlensing surveys, which extend to $∼10$ [ref] .
Subaru through a different lens: microlensing by extended dark matter structures · aLIGO sensitivity to compact objects · 0.93
Cites as background 1 paper
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The characteristic strain during the inspiral phase in the quadrupole approximation is given by (see, e.g. [ref] ) [equation] Here $θ$ is the angle between the normal to the orbit and the line of sight, $d$ is the distance to the source, and the phases $Ψ_×= Ψ_+ + π/2$ are given by [equation] with $Φ_0$ the value of the common phase $Φ$ at the time of coalescence $t_c$.
The basics of gravitational wave theory · Gravitational waves from compact object mergers · 0.89
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