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Probing the interaction between dark energy and dark matter with future fast radio burst observations
Cosmology and Nongalactic Astrophysics · Submitted 13 Oct 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In all the IDE models, about $10^6$ FRB data can achieve the absolute errors of $\beta$ to less than $0.10$, providing a way to precisely measure $\beta$ by only one cosmological probe.
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The abstract, sentence by sentence
Interacting dark energy (IDE) scenario assumes that there exists a direct interaction between dark energy and cold dark matter, but this interaction is hard to be tightly constrained by the current data. Fast radio bursts (FRBs) will be seen in large numbers by future radio telescopes, and thus they have potential to become a promising low-redshift cosmological probe. In this work, we investigate the capability of future FRBs of constraining the dimensionless coupling parameter $\beta$ in four phenomenological IDE models. If we fix the FRB properties, about $10^5$ FRB data can give constraints on $\beta$ tighter than the current cosmic microwave background data in the IDE models with the interaction proportional to the energy density of dark energy. In all the IDE models, about $10^6$ FRB data can achieve the absolute errors of $\beta$ to less than $0.10$, providing a way to precisely measure $\beta$ by only one cosmological probe. Jointly constraining the FRB properties and cosmological parameters would increase the constraint errors of $\beta$ by a factor of about 0.5-2.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Interacting dark energy (IDE) scenario assumes that there exists a direct interaction between dark energy and cold dark matter, but this interaction is hard to be tightly constrained by the current data. | background 0.63 | 0.04 | 0.02 | asserted 0.98 |
| s1 | Fast radio bursts (FRBs) will be seen in large numbers by future radio telescopes, and thus they have potential to become a promising low-redshift cosmological probe. | background 0.99 | 0.06 | 0.03 | hedged possibility 0.84 |
| s2 | In this work, we investigate the capability of future FRBs of constraining the dimensionless coupling parameter $\beta$ in four phenomenological IDE models. | contribution 1.00 | 0.84 | 0.08 | asserted 0.88 |
| s3 | If we fix the FRB properties, about $10^5$ FRB data can give constraints on $\beta$ tighter than the current cosmic microwave background data in the IDE models with the interaction proportional to the energy density of dark energy. | result 1.00 | 0.76 | 0.22 | hedged possibility 0.62 |
| s4 | In all the IDE models, about $10^6$ FRB data can achieve the absolute errors of $\beta$ to less than $0.10$, providing a way to precisely measure $\beta$ by only one cosmological probe. | result 0.99 | 0.82 | 0.57 | asserted 0.86 |
| s5 | Jointly constraining the FRB properties and cosmological parameters would increase the constraint errors of $\beta$ by a factor of about 0.5-2. | result 0.95 | 0.79 | 0.08 | asserted 0.92 |
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The paper
Original abstract
Interacting dark energy (IDE) scenario assumes that there exists a direct interaction between dark energy and cold dark matter, but this interaction is hard to be tightly constrained by the current data. Fast radio bursts (FRBs) will be seen in large numbers by future radio telescopes, and thus they have potential to become a promising low-redshift cosmological probe. In this work, we investigate the capability of future FRBs of constraining the dimensionless coupling parameter $\beta$ in four phenomenological IDE models. If we fix the FRB properties, about $10^5$ FRB data can give constraints on $\beta$ tighter than the current cosmic microwave background data in the IDE models with the interaction proportional to the energy density of dark energy. In all the IDE models, about $10^6$ FRB data can achieve the absolute errors of $\beta$ to less than $0.10$, providing a way to precisely measure $\beta$ by only one cosmological probe. Jointly constraining the FRB properties and cosmological parameters would increase the constraint errors of $\beta$ by a factor of about 0.5-2.
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References
How the literature uses it
10 arXiv papers cite this in 10 sentences
Papers citing it · 5 sentences without a confident label
Cites it as support 1 paper
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Actually, the IDECAMB code for the CF models has been widely tested in our recent works [ref] .
IDECAMB: an implementation of interacting dark energy cosmology in CAMB · Constraints on a specific model · 0.97
Cites it as background 4 papers
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Another assumption posits $Q$ as $Q=βH_0 ρ_c$ or $Q=βH_0 ρ_de$ [ref] , with the Hubble constant $H_0$ used for dimensional consistency.
Prospects for weighing neutrinos in interacting dark energy models using joint observations of gravitational waves and $\gamma$-ray bursts · Introduction · 0.92
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Interacting dark energy (IDE) models have garnered substantial attention [ref] .
Revisiting holographic dark energy after DESI 2024 · Introduction · 0.90
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While systematics-based explanations (e.g. Refs. [ref] ) are not yet completely excluded (but are admittedly becoming increasingly unlikely), the possibility of the Hubble tension calling for new physics, potentially related to the dark sector, is now taken very seriously, with a wide range of proposals having been put forward: with no claims as to completeness, see e.g. Refs. [ref] for examples of the rich variety of discussions in this context, as well as approaches adopted, with varying degrees of success.
Seven hints that early-time new physics alone is not sufficient to solve the Hubble tension · Introduction · 0.96
What it cites · 83 sentences without a confident label
Uses the method or tool of 2 papers
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We use the modified CAMB [ref] and cosmomc codes [ref] with the inclusion of the ePPF module and obtain the posterior probability distribution of cosmological parameters.
Cosmological parameters from CMB and other data: a Monte-Carlo approach · Cosmological data · 1.00
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We use the modified CAMB [ref] and cosmomc codes [ref] with the inclusion of the ePPF module and obtain the posterior probability distribution of cosmological parameters.
Efficient Computation of CMB anisotropies in closed FRW models · Cosmological data · 1.00
Uses data or values from 9 papers
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[ref] , [equation] where the top hat model for halos’ gas profile of the ionized baryons is assumed.
Locating the "missing" baryons with extragalactic dispersion measure estimates · Mock FRB data · 0.89
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For the current cosmological data as comparison, we use the Planck 2018 CMB “distance priors" [ref] , and the baryon acoustic oscillation (BAO) measurements from 6dFGS at $z_eff = 0.106$ [ref] , SDSS-MGS at $z_eff = 0.15$ [ref] , and BOSS-DR12 at $z_eff = 0.38$, 0.51, and 0.61 [ref] .
The 6dF Galaxy Survey: Baryon Acoustic Oscillations and the Local Hubble Constant · Cosmological data · 0.92
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For the current cosmological data as comparison, we use the Planck 2018 CMB “distance priors" [ref] , and the baryon acoustic oscillation (BAO) measurements from 6dFGS at $z_eff = 0.106$ [ref] , SDSS-MGS at $z_eff = 0.15$ [ref] , and BOSS-DR12 at $z_eff = 0.38$, 0.51, and 0.61 [ref] .
The Clustering of the SDSS DR7 Main Galaxy Sample I: A 4 per cent Distance Measure at z=0.15 · Cosmological data · 0.92
Cites as background 24 papers
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A lot of works have proposed that the FRB data can constrain cosmological parameters [ref] and related parameters [ref] .
Consistent Constraints on the Equivalence Principle from localised Fast Radio Bursts · Introduction · 0.80
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A lot of works have proposed that the FRB data can constrain cosmological parameters [ref] and related parameters [ref] .
A path to precision cosmology: synergy between four promising late-universe cosmological probes · Introduction · 0.80
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A lot of works have proposed that the FRB data can constrain cosmological parameters [ref] and related parameters [ref] .
Improvement of cosmological constraints with the cross correlation between line-of-sight optical galaxy and FRB dispersion measure · Introduction · 0.80
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