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Prospects for weighing neutrinos in interacting dark energy models using joint observations of gravitational waves and $\gamma$-ray bursts
Cosmology and Nongalactic Astrophysics · Submitted 30 Apr 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This indicates that in the context of IDE models, the improvement in neutrino mass constraints from GW observations is relatively limited.
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The abstract, sentence by sentence
Cosmological observations can be used to weigh neutrinos, but this method is model-dependent, with results relying on the cosmological model considered. If we consider interactions between dark energy and dark matter, the neutrino mass constraints differ from those derived under the standard model. On the contrary, gravitational wave (GW) standard siren observations can measure absolute cosmological distances, helping to break parameter degeneracies inherent in traditional cosmological observations, thereby improving constraints on neutrino mass. This paper examines the constraints on neutrino mass within interacting dark energy (IDE) models and explores how future GW standard siren observations could enhance these results. For multi-messenger GW observations, we consider the joint observations of binary neutron star mergers by third-generation ground-based GW detectors and short $\gamma$-ray burst observations by missions similar to the THESEUS satellite project. Using current cosmological observations (CMB+BAO+SN), we obtain an upper limit on the neutrino mass in the IDE models of 0.15 (or 0.16) eV. With the inclusion of GW data, the upper limit on the neutrino mass improves to 0.14 eV. This indicates that in the context of IDE models, the improvement in neutrino mass constraints from GW observations is relatively limited. However, GW observations significantly enhance the constraints on other cosmological parameters, such as matter density parameter, the Hubble constant, and coupling strength between dark energy and dark matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Cosmological observations can be used to weigh neutrinos, but this method is model-dependent, with results relying on the cosmological model considered. | background 0.98 | 0.05 | 0.03 | asserted 0.94 |
| s1 | If we consider interactions between dark energy and dark matter, the neutrino mass constraints differ from those derived under the standard model. | background 0.98 | 0.10 | 0.06 | asserted 0.82 |
| s2 | On the contrary, gravitational wave (GW) standard siren observations can measure absolute cosmological distances, helping to break parameter degeneracies inherent in traditional cosmological observations, thereby improving constraints on neutrino mass. | background 0.89 | 0.08 | 0.11 | asserted 0.89 |
| s3 | This paper examines the constraints on neutrino mass within interacting dark energy (IDE) models and explores how future GW standard siren observations could enhance these results. | contribution 1.00 | 0.63 | 0.08 | asserted 0.86 |
| s4 | For multi-messenger GW observations, we consider the joint observations of binary neutron star mergers by third-generation ground-based GW detectors and short $\gamma$-ray burst observations by missions similar to the THESEUS satellite project. | method 0.99 | 0.51 | 0.03 | asserted 0.93 |
| s5 | Using current cosmological observations (CMB+BAO+SN), we obtain an upper limit on the neutrino mass in the IDE models of 0.15 (or 0.16) eV. | result 0.99 | 0.89 | 0.11 | asserted 1.00 |
| s6 | With the inclusion of GW data, the upper limit on the neutrino mass improves to 0.14 eV. | result 1.00 | 0.88 | 0.18 | asserted 1.00 |
| s7 | This indicates that in the context of IDE models, the improvement in neutrino mass constraints from GW observations is relatively limited. | interpretation 0.96 | 0.86 | 0.33 | hedged possibility 0.88 |
| s8 | However, GW observations significantly enhance the constraints on other cosmological parameters, such as matter density parameter, the Hubble constant, and coupling strength between dark energy and dark matter. | result 0.86 | 0.82 | 0.20 | asserted 1.00 |
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The paper
Original abstract
Cosmological observations can be used to weigh neutrinos, but this method is model-dependent, with results relying on the cosmological model considered. If we consider interactions between dark energy and dark matter, the neutrino mass constraints differ from those derived under the standard model. On the contrary, gravitational wave (GW) standard siren observations can measure absolute cosmological distances, helping to break parameter degeneracies inherent in traditional cosmological observations, thereby improving constraints on neutrino mass. This paper examines the constraints on neutrino mass within interacting dark energy (IDE) models and explores how future GW standard siren observations could enhance these results. For multi-messenger GW observations, we consider the joint observations of binary neutron star mergers by third-generation ground-based GW detectors and short $\gamma$-ray burst observations by missions similar to the THESEUS satellite project. Using current cosmological observations (CMB+BAO+SN), we obtain an upper limit on the neutrino mass in the IDE models of 0.15 (or 0.16) eV. With the inclusion of GW data, the upper limit on the neutrino mass improves to 0.14 eV. This indicates that in the context of IDE models, the improvement in neutrino mass constraints from GW observations is relatively limited. However, GW observations significantly enhance the constraints on other cosmological parameters, such as matter density parameter, the Hubble constant, and coupling strength between dark energy and dark matter.
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References
How the literature uses it
11 arXiv papers cite this in 17 sentences
Papers whose main result relates to this one's
States the same result 1 paper
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We find that the GW standard siren observations from ET and CE can only slightly improve the constraint on the neutrino mass in the IDE models, compared to the current limit.
Papers citing it · 8 sentences without a confident label
Uses its method or tool 1 paper
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We use the simulation method as prescribed in Refs. [ref] .
Prospects for searching for sterile neutrinos with gravitational wave and $\gamma$-ray burst joint observations · Gravitational wave simulation · 1.00
Cites it as background 8 papers
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If the redshift information could also be obtained by identifying electromagnetic (EM) counterparts (this type of standard sirens are typically referred to as “bright sirens”) or statistically from cross-matching of GW and galaxy catalogs (this type of standard sirens are typically referred to as “dark sirens”), the distance-redshift relation could be used to explore the expansion history of the universe, which is widely discussed in the literature [ref] .
Standard siren cosmology in the era of the 2.5-generation ground-based gravitational wave detectors: bright and dark sirens of LIGO Voyager and NEMO · Introduction · 0.88
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Gravitational-wave (GW) standard sirens provide an absolute distance indicator that does not rely on the traditional distance ladder, as the waveform amplitude of compact binary coalescences directly encodes the luminosity distance [ref] .
Model-independent H0 from GWTC-4 standard sirens and TDCOSMO 2025 strong lensing time delays · Introduction · 0.90
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Additionally, neutrinos, as a unique relativistic component of the universe, play a non-negligible role in the cosmic expansion history and the formation of large-scale structures at late times [ref] .
Neutrino mass constraints in interacting dark energy models after DESI DR2 · Introduction · 0.86
What it cites · 78 sentences without a confident label
Uses the method or tool of 16 papers
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Under such a circumstance, to avoid the perturbation instability problem in the I$Λ$CDM model, in this work, we treat the vacuum energy perturbations based on the extended parameterized post-Friedmann (PPF) approach [ref] (for the original version of the PPF method, see Refs. [ref] ).
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Under such a circumstance, to avoid the perturbation instability problem in the I$Λ$CDM model, in this work, we treat the vacuum energy perturbations based on the extended parameterized post-Friedmann (PPF) approach [ref] (for the original version of the PPF method, see Refs. [ref] ).
Crossing the Phantom Divide with Parameterized Post-Friedmann Dark Energy · Methodology · 0.99
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Under such a circumstance, to avoid the perturbation instability problem in the I$Λ$CDM model, in this work, we treat the vacuum energy perturbations based on the extended parameterized post-Friedmann (PPF) approach [ref] (for the original version of the PPF method, see Refs. [ref] ).
Parametrized Post-Friedmann Signatures of Acceleration in the CMB · Methodology · 0.99
Uses data or values from 12 papers
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We found that only approximately 640 standard sirens can be detected for the ET2CE+THESEUS network in 10 years, whose redshift distribution is given in Ref. [ref] .
A comprehensive forecast for cosmological parameter estimation using joint observations of gravitational waves and short $\gamma$-ray bursts · Results and discussion · 0.98
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For the CMB data, we use the CMB likelihood, including the TT, TE, and EE spectra at $l≥30$, low-$l$ temperature commander likelihood, and low-$l$ SimAll EE likelihood, from the Planck 2018 data release [ref] .
Planck 2018 results. VI. Cosmological parameters · Methodology · 0.99
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The overall normalization is fixed by requiring that the value of $ℛ_m(z=0)=920 Gpc^-3 yr^-1$ agrees with the local rate estimated from the O1 LIGO and O2 LIGO/Virgo observation run [ref] , which is also in accordance with the latest O3 observation run [ref] . $P(t_d)$ is the distribution of the time delay $t_d$, and we follow and adopt the exponential form [ref] [equation] with an e-fold time of $τ=100$ Myr for $t_d>t_min=20$ Myr.
The population of merging compact binaries inferred using gravitational waves through GWTC-3 · Methodology · 0.94
Cites as background 20 papers
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In the coming decades, third-generation (3G) ground-based GW detectors, such as Cosmic Explorer (CE) [ref] and Einstein Telescope (ET) [ref] , are set to revolutionize the measurement of GW signals.
Exploring the Sensitivity of Next Generation Gravitational Wave Detectors · Introduction · 0.89
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In the field of IDE, one common assumption is that $Q$ is proportional to the density of either dark matter or dark energy, i.e., $Q=βH ρ_c$ or $Q=βH ρ_de$ [ref] , where $β$ is a dimensionless coupling parameter and $H$ facilitates computational ease.
Exploring interacting holographic dark energy in a perturbed universe with parameterized post-Friedmann approach · Introduction · 0.88
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In the field of IDE, one common assumption is that $Q$ is proportional to the density of either dark matter or dark energy, i.e., $Q=βH ρ_c$ or $Q=βH ρ_de$ [ref] , where $β$ is a dimensionless coupling parameter and $H$ facilitates computational ease.
Models of vacuum energy interacting with cold dark matter: Constraints and comparison · Introduction · 0.88
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