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Consequences of dark matter-dark energy interaction on cosmological parameters derived from SNIa data
Astrophysics · Submitted 26 Oct 2006
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Thus, an independent measurement of the present dark matter density can place constraints on models with interacting dark energy.
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
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The abstract, sentence by sentence
Models where the dark matter component of the universe interacts with the dark energy field have been proposed as a solution to the cosmic coincidence problem, since in the attractor regime both dark energy and dark matter scale in the same way. In these models the mass of the cold dark matter particles is a function of the dark energy field responsible for the present acceleration of the universe, and different scenarios can be parameterized by how the mass of the cold dark matter particles evolves with time. In this article we study the impact of a constant coupling $\delta$ between dark energy and dark matter on the determination of a redshift dependent dark energy equation of state $w_{DE}(z)$ and on the dark matter density today from SNIa data. We derive an analytical expression for the luminosity distance in this case. In particular, we show that the presence of such a coupling increases the tension between the cosmic microwave background data from the analysis of the shift parameter in models with constant $w_{DE}$ and SNIa data for realistic values of the present dark matter density fraction. Thus, an independent measurement of the present dark matter density can place constraints on models with interacting dark energy.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Models where the dark matter component of the universe interacts with the dark energy field have been proposed as a solution to the cosmic coincidence problem, since in the attractor regime both dark energy and dark matter scale in the same way. | background 1.00 | 0.04 | 0.03 | asserted 0.84 |
| s1 | In these models the mass of the cold dark matter particles is a function of the dark energy field responsible for the present acceleration of the universe, and different scenarios can be parameterized by how the mass of the cold dark matter particles evolves with time. | background 1.00 | 0.04 | 0.02 | asserted 0.99 |
| s2 | In this article we study the impact of a constant coupling $\delta$ between dark energy and dark matter on the determination of a redshift dependent dark energy equation of state $w_{DE}(z)$ and on the dark matter density today from SNIa data. | contribution 0.99 | 0.90 | 0.07 | asserted 0.89 |
| s3 | We derive an analytical expression for the luminosity distance in this case. | method 0.76 | 0.96 | 0.03 | asserted 0.99 |
| s4 | In particular, we show that the presence of such a coupling increases the tension between the cosmic microwave background data from the analysis of the shift parameter in models with constant $w_{DE}$ and SNIa data for realistic values of the present dark matter density fraction. | result 0.98 | 0.91 | 0.61 | asserted 1.00 |
| s5 | Thus, an independent measurement of the present dark matter density can place constraints on models with interacting dark energy. | interpretation 0.97 | 0.42 | 0.54 | asserted 0.52 |
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The paper
Original abstract
Models where the dark matter component of the universe interacts with the dark energy field have been proposed as a solution to the cosmic coincidence problem, since in the attractor regime both dark energy and dark matter scale in the same way. In these models the mass of the cold dark matter particles is a function of the dark energy field responsible for the present acceleration of the universe, and different scenarios can be parameterized by how the mass of the cold dark matter particles evolves with time. In this article we study the impact of a constant coupling $\delta$ between dark energy and dark matter on the determination of a redshift dependent dark energy equation of state $w_{DE}(z)$ and on the dark matter density today from SNIa data. We derive an analytical expression for the luminosity distance in this case. In particular, we show that the presence of such a coupling increases the tension between the cosmic microwave background data from the analysis of the shift parameter in models with constant $w_{DE}$ and SNIa data for realistic values of the present dark matter density fraction. Thus, an independent measurement of the present dark matter density can place constraints on models with interacting dark energy.
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References
How the literature uses it
52 arXiv papers cite this in 69 sentences
Papers citing it · 34 sentences without a confident label
Compares with it 4 papers
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Amendola - 1999 [ref] $ρ̇_m+3 H ρ_m=-C ρ_m ϕ̇$ Yes Amendola - 1999 [ref] $ρ̇_m+3 H ρ_m=-C ρ_m ϕ̇$ Yes Billyard & Coley -1999 [ref] $ϕ̇(ϕ̈+3 H ϕ̇+k V)=(4-3 γ)/2 √(ω+3/2) ϕ̇ μ$ Yes Olivares.etal - 2005 [ref] $d ρ_c/d t+3 H ρ_c=3 H c^2(ρ_c+ρ_x)$ No Amendola.etal - 2006 [ref] $ρ̇_D M+3 H ρ_D M-δ(a) H ρ_D M=0$ No Olivares.etal - 2007 [ref] $ρ̇_c+3 H ρ_c=3 H c^2(ρ_x+ρ_c)$ No 2*Boehmer.etal - 2008 [ref] $ρ̇_c+3 H ρ_c=-√(2 / 3) κβρ_c φ̇$ Yes $ρ̇_c+3 H ρ_c=-αH ρ_c$ No 2*Caldera-Cabral.etal - 2008 [ref] $ρ̇_c=-3 H ρ_c+3 H(α_x ρ_x+α_c ρ_c)$ No $ρ̇_c=-3 H ρ_c+3(Γ_x ρ_x+Γ_c ρ_c)$ No 2*He & Wang - 2008 [ref] $ρ̇_D M+3 H ρ_D M-δH ρ_D M=0$ No $ρ̇_D M+3 H ρ_D M-δH (ρ_D M+ρ_DE)=0$ No Pettorino & Baccigalupi - 2008 [ref] $ϕ^''+2 ℋ ϕ^'+a^2 U_, ϕ=a^2 C_c ρ_c$ Yes Quartin.etal - 2008 [ref] $d ρ_c/d N+3 ρ_c=3λ_x ρ_x+λ_c ρ_c$ No 3*Boehmer.etal - 2009 [ref] $ρ̇_c=-3 H ρ_c-α/M_0 ρ_φ^2$ No $ρ̇_c=-3 H ρ_c-β/M_0 ρ_c
Cosmological perturbations in the interacting dark sector: Mapping fields and fluids · Interacting dark energy models in the literature · 0.91
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These results are consistent with those found in the literature, see for instance Ref. [ref] for null coupling ($_dm=0.37^+0.06_-0.08$) or with the result obtained in Ref. [ref] , ($_dm=0.30^+0.17_-0.07$) through mean relative peculiar velocity measurements for pairs of galaxies.
Unified model of baryonic matter and dark components · CONCLUSIONS · 0.98
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Note that Ansatz [ref] resembles Eq. (8) of Ref. [ref] with $Γ_VV ≡1/τ0$ and Eq. (3) of Ref. [ref] , but differs by points 1 and 2, respectively.
Equilibrium boundary conditions, dynamic vacuum energy, and the Big Bang · Additional remarks · 1.00
Cites it as background 25 papers
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Many DDE models are designed to solve the coincidence problem by having $ρ_de(t) ∼ρ_m(t)$ for a large fraction of the history/future of the universe [ref] .
Dark-Energy Dynamics Required to Solve the Cosmic Coincidence · Introduction · 0.83
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On one side, within the usual framework of General Relativity (Einstein Frame, EF) the effect of a coupling between dark energy and dark matter (Coupled Quintessence, CQ) has been deeply investigated both in the linear [ref] and non-linear regimes [ref] , including the effects of such models on the Cosmic Microwave Background (CMB) [ref] , on Supernovae [ref] , on the matter power spectrum [ref] , on structure formation [ref] , also via N-body simulation [ref] , as well as different choices of the coupling [ref] .
Coupled and Extended Quintessence: theoretical differences and structure formation · Introduction · 1.00
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A number of studies have been devoted to analyze the constraints from Cosmic Microwave Background (CMB), large scale structure (LSS), Supernovae Ia and Baryon Acoustic oscillations (BAO) on a variety of interacting models [ref] .
Coupled dark matter-dark energy in light of near Universe observations · Introduction · 0.89
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