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Impacts of new small-scale N-body simulations on dark matter annihilations constrained from cosmological 21cm line observations
Cosmology and Nongalactic Astrophysics · Submitted 27 Mar 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim By assuming the thermal freezeout scenario, we find that $m_{\rm DM} < 15$ GeV and $m_{\rm DM} < 3$ GeV have been excluded at 95$\%$ C.L. for the annihilation modes into $b\bar{b}$ and $e^+ e^-$, respectively.
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The abstract, sentence by sentence
We revisit constraints on annihilating dark matter based on the global 21cm signature observed by EDGES. For this purpose, we used the numerical data of the latest N-body simulation performed by state-of-the-art standard in order to estimate the boost factor at high redshifts ($z$ = 10 - 100), which enhances the annihilation of dark matter in course of structure formation. By taking into account to what fraction injected energy from dark matter annihilation contributes to ionization, excitation and heating of intergalactic medium during dark ages, we estimated how large the global 21cm absorption can be. By assuming the thermal freezeout scenario, we find that $m_{\rm DM} < 15$ GeV and $m_{\rm DM} < 3$ GeV have been excluded at 95$\%$ C.L. for the annihilation modes into $b\bar{b}$ and $e^+ e^-$, respectively.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We revisit constraints on annihilating dark matter based on the global 21cm signature observed by EDGES. | contribution 0.72 | 0.58 | 0.03 | asserted 0.59 |
| s1 | For this purpose, we used the numerical data of the latest N-body simulation performed by state-of-the-art standard in order to estimate the boost factor at high redshifts ($z$ = 10 - 100), which enhances the annihilation of dark matter in course of structure formation. | method 0.99 | 0.76 | 0.03 | asserted 0.96 |
| s2 | By taking into account to what fraction injected energy from dark matter annihilation contributes to ionization, excitation and heating of intergalactic medium during dark ages, we estimated how large the global 21cm absorption can be. | method 0.99 | 0.91 | 0.04 | asserted 0.97 |
| s3 | By assuming the thermal freezeout scenario, we find that $m_{\rm DM} < 15$ GeV and $m_{\rm DM} < 3$ GeV have been excluded at 95$\%$ C.L. for the annihilation modes into $b\bar{b}$ and $e^+ e^-$, respectively. | result 1.00 | 0.94 | 0.89 | asserted 1.00 |
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The paper
Original abstract
We revisit constraints on annihilating dark matter based on the global 21cm signature observed by EDGES. For this purpose, we used the numerical data of the latest N-body simulation performed by state-of-the-art standard in order to estimate the boost factor at high redshifts ($z$ = 10 - 100), which enhances the annihilation of dark matter in course of structure formation. By taking into account to what fraction injected energy from dark matter annihilation contributes to ionization, excitation and heating of intergalactic medium during dark ages, we estimated how large the global 21cm absorption can be. By assuming the thermal freezeout scenario, we find that $m_{\rm DM} < 15$ GeV and $m_{\rm DM} < 3$ GeV have been excluded at 95$\%$ C.L. for the annihilation modes into $b\bar{b}$ and $e^+ e^-$, respectively.
Human review
How the literature uses it
6 arXiv papers cite this in 11 sentences
Papers citing it · 9 sentences without a confident label
Uses its method or tool 1 paper
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The BF can be obtained by directly integrating the nonlinear matter power spectrum for investigated scales at different redshifts [ref] .
Influence of the deviation of the matter power spectrum at small scales on the global 21-cm signal at cosmic dawn · The matter power spectrum at small scales and the evolution of IGM · 0.97
Cites it as background 1 paper
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On the other hand, the global 21-cm signal can be used to investigate the properties of DM; see, e.g, Refs [ref] .
Influence of the deviation of the matter power spectrum at small scales on the global 21-cm signal at cosmic dawn · introduction · 0.92
What it cites · 26 sentences without a confident label
Uses the method or tool of 11 papers
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In this paper, we adopt the results of [ref] [<https://faun.rc.fas.harvard.edu/epsilon/>], which treats the effects of energy injection at linear level.
Indirect Dark Matter Signatures in the Cosmic Dark Ages II. Ionization, Heating and Photon Production from Arbitrary Energy Injections · Energy injection and deposition into IGM from DM annihilation · 0.94
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We in particular obtain conservative upper bounds on DM annihilation cross section by maximizing absorption amplitude in the absence of DM annihilation [ref] .
Bounds on Dark Matter annihilations from 21 cm data · Results · 0.91
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In numerical calculation we present in Section [ref], we adopt the recombination code HyRec[<https://pages.jh.edu/ yalihai1/hyrec/hyrec.html>], which is based on the state-of-art effective multi-level atom (See [ref] for details).
HyRec: A fast and highly accurate primordial hydrogen and helium recombination code · Evolution equations of IGM in the presence of energy injection · 1.00
Uses data or values from 1 paper
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The fact that EDGES has reported a global absorption signal [ref] T_21cm=- 500^+200_-500 mK (), indicating $T_m<T_γ$ and upper bounds on DM annihilation.
An absorption profile centred at 78 megahertz in the sky-averaged spectrum · Results · 0.90
Compares with 2 papers
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That is because the boost factor we adopted is smaller than the ones in [ref] .
Bounds on Dark Matter annihilations from 21 cm data · Results · 1.00
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As reference, the figure also shows $B(z)$ computed based on linear perturbation theory as well as one based on the halo model in [ref] , which is referred as the "Boost 1" model in [ref] .
Unveiling the nature of dark matter with high redshift 21 cm line experiments · N-body simulation and the annihilation boost factor · 0.96
Cites as support 1 paper
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Then, the energy-deposition is more efficient for $W^+W^-$ and $bb̅$ due to the delayed deposition [ref] .
Too Hot, Too Cold or Just Right? Implications of a 21-cm Signal for Dark Matter Annihilation and Decay · Results · 0.97
Cites as background 26 papers
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In scenarios of dark matter (DM) for the weakly-interacting massive particle (WIMP) [ref] , a DM particle with mass of the weak scale should have a thermally-averaged annihilation cross section of the order of $⟨σv ⟩= 2 ×10^26 cm^3/sec$ [ref] .
Precise WIMP Dark Matter Abundance and Standard Model Thermodynamics · Introduction · 0.81
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In scenarios of dark matter (DM) for the weakly-interacting massive particle (WIMP) [ref] , a DM particle with mass of the weak scale should have a thermally-averaged annihilation cross section of the order of $⟨σv ⟩= 2 ×10^26 cm^3/sec$ [ref] .
Precise Relic WIMP Abundance and its Impact on Searches for Dark Matter Annihilation · Introduction · 0.81
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In scenarios of dark matter (DM) for the weakly-interacting massive particle (WIMP) [ref] , a DM particle with mass of the weak scale should have a thermally-averaged annihilation cross section of the order of $⟨σv ⟩= 2 ×10^26 cm^3/sec$ [ref] .
Supersymmetric Dark Matter · Introduction · 0.81
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