Papers › Bound Dark Energy: towards understanding the nature of the Dark Energy
Bound Dark Energy: towards understanding the nature of the Dark Energy
Erick Almaraz, Axel de la Macorra
The archive published only this paper's code-link row. Authors, date and abstract are from arXiv's metadata (CC0), read from the Kaggle arXiv metadata snapshot of 2026-09-12 where its title matched the archive's; the title is the archive's.
We present a complete analysis of the observational constraints and cosmological implications of our Bound Dark Energy (BDE) model aimed to explain the late-time cosmic acceleration of the universe. BDE is derived from particle physics and corresponds to the lightest meson field ϕ dynamically formed at low energies due to the strong gauge coupling constant. The evolution of the dark energy is determined by the scalar potential V(ϕ)=Λ_c^(4+2/3)ϕ^(-2/3) arising from non-perturbative effects at a condensation scale Λ_c and scale factor a_c, related each other by a_cΛ_c/eV=1.0934×10⁻⁴. We present the full background and perturbation evolution at a linear level. Using current observational data, we obtain the constraints a_c=(2.48 ±0.02)×10⁻⁶ and Λ_c=(44.09 ±0.28) eV, which is in complete agreement with our theoretical prediction Λ_cᵗʰ=34⁺¹⁶₋₁₁ eV. The bounds on the equation of state today, the dark energy density and the expansion rate are w_(BDE 0)=-0.929±0.007, Ω_(BDE0)=0.696±0.007 and H₀=67.82±0.05 km s⁻¹Mpc, respectively. Even though the constraints on the six Planck base parameters are consistent at the 1σ level between BDE and the concordance ΛCDM model, BDE improves the likelihood ratio by 2.1 of the Baryon Acoustic Oscillations (BAO) measurements with respect to ΛCDM and has an equivalent fit for type Ia supernovae and the Cosmic Microwave Background data. We present the constraints on the different cosmological parameters, and particularly we show the tension between BDE and ΛCDM in the BAO distance ratio r_(BAO) vs H₀ and the growth index γ at different redshifts, as well as the dark matter density at present time Ω_ch² vs H₀.
Code
Repository list and official/mentioned flags are the archive's, frozen 2025-07-28. Reachability, where shown, is from one Syntology probe window (2026-09-16 to 2026-09-18); repositories not probed show nothing. GitHub stars are not tracked.
Code Syntology ran Syntology
Not run by Syntology. Nothing on this page verifies that the listed code works.
Results from the paper archive 2025-07-28
No leaderboard rows for this paper in the archive.
Report a problem or propose a change · a person checks every report against the paper or source before anything changes; decisions are listed on /corrections