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Dark Energy within the Generalized Uncertainty Principle in Light of DESI DR2

Andronikos Paliathanasis

TL;DR

This paper investigates a GUP-based deformation of ΛCDM by modifying the Raychaudhuri equation through a deformed algebra, producing a dynamical dark energy description with a single additional degree of freedom characterized by β. Focusing on a quadratic GUP, the authors derive a closed-form asymptotic Hubble function and formulate a modified Hubble evolution that reduces to ΛCDM as β→0, while introducing β-dependent corrections that alter late-time dynamics. They constrain the model with Pantheon+ SNIa, cosmic chronometers, and DESI BAO data (2024 and 2025 releases), finding β is negative and that BAO data modestly favor the GUP-modified model, with Bayesian evidence strengthening upon including the DESI 2025 release; AIC results are largely inconclusive. Overall, the work provides a viable dynamical dark energy mechanism anchored in quantum gravity-inspired GUP effects and highlights the potential of upcoming BAO data to sharpen distinctions from ΛCDM.

Abstract

In this study, we modify the $Λ$CDM model by introducing a deformed algebra within the framework of the Generalized Uncertainty Principle (GUP). We formulate the modified Raychaudhuri equation, where new terms are introduced which describe dynamical pressure components. For the quadratic GUP model, we derive the Hubble function, which leads to a time-dependent dark energy model. The free parameters are determined using late-time observational data, the Pantheon+ SNIa sample, the cosmic chronometers, and the DESI 2025 BAO data. We find that the modified model introduce only one new additional degree of freedom compared to the $Λ$CDM model. The GUP-Modified $Λ$CDM model provides a better fit to the data than the undeformed theory. Furthermore, we compare the same model with the DESI 2024 BAO data and find that the Bayesian evidence becomes stronger with the inclusion of the DESI 2025 release.

Dark Energy within the Generalized Uncertainty Principle in Light of DESI DR2

TL;DR

This paper investigates a GUP-based deformation of ΛCDM by modifying the Raychaudhuri equation through a deformed algebra, producing a dynamical dark energy description with a single additional degree of freedom characterized by β. Focusing on a quadratic GUP, the authors derive a closed-form asymptotic Hubble function and formulate a modified Hubble evolution that reduces to ΛCDM as β→0, while introducing β-dependent corrections that alter late-time dynamics. They constrain the model with Pantheon+ SNIa, cosmic chronometers, and DESI BAO data (2024 and 2025 releases), finding β is negative and that BAO data modestly favor the GUP-modified model, with Bayesian evidence strengthening upon including the DESI 2025 release; AIC results are largely inconclusive. Overall, the work provides a viable dynamical dark energy mechanism anchored in quantum gravity-inspired GUP effects and highlights the potential of upcoming BAO data to sharpen distinctions from ΛCDM.

Abstract

In this study, we modify the CDM model by introducing a deformed algebra within the framework of the Generalized Uncertainty Principle (GUP). We formulate the modified Raychaudhuri equation, where new terms are introduced which describe dynamical pressure components. For the quadratic GUP model, we derive the Hubble function, which leads to a time-dependent dark energy model. The free parameters are determined using late-time observational data, the Pantheon+ SNIa sample, the cosmic chronometers, and the DESI 2025 BAO data. We find that the modified model introduce only one new additional degree of freedom compared to the CDM model. The GUP-Modified CDM model provides a better fit to the data than the undeformed theory. Furthermore, we compare the same model with the DESI 2024 BAO data and find that the Bayesian evidence becomes stronger with the inclusion of the DESI 2025 release.

Paper Structure

This paper contains 11 sections, 45 equations, 4 figures, 3 tables.

Table of Contents

  1. Introduction
  2. Generalized Uncertainty Principle
  3. $\Lambda$-Cosmology with GUP-Modified Raychaudhuri Equation
  4. GUP-Modified Field Equations
  5. Asymptotic dynamics
  6. Quadratic GUP: $f\left( t\right) \simeq P^{2}\rho_{m}^{-\frac{7}{3}}$
  7. Observational Data Analysis
  8. Reference model and information criteria
  9. Results
  10. Conclusions
  11. Constant function $f\left( t\right) =1$

Figures (4)

  • Figure 1: Qualitative evolution for the equation of state parameter $w_{DE}\left( a\right)$ for the GUP-modified $\Lambda$CDM model (\ref{['fe.29a']}) and (\ref{['fe.33a']}) for different values of parameter $\beta$. Solid line is for the$~\Lambda$CDM universe, dotted line is for $\beta=-0.01$ and dashed line is for $\beta=+0.01$. For the plot we considered $\Omega_{m0}=0.3$. The transition point where the $w_{DE}\left( a\right)$ crosses the phantom divide line depends on parameter $\Omega_{m0}.$ For larger values of $\Omega_{m0}$ tthe transition point occurs at lower redshifts, while for smaller values of $\Omega_{m0}$ it shifts to higher redshifts.
  • Figure 2: Qualitative evolution for the effective equation of state parameter $w_{eff}\left( a\right)$ for the GUP-Modified $\Lambda$CDM model (\ref{['fe.29a']}) for different values of parameter $\beta$. Gray area is for $\beta\in\left[ -0.05,+0.05\right]$. Solid line is for the$~\Lambda$CDM universe, dotted line is for $\beta=-0.01$ and dashed line is for $\beta=+0.01$. For the plot we considered $\Omega_{m0}=0.3$.
  • Figure 3: Confidence space for the best-fit parameters for the GUP-modified model with Hubble function (\ref{['fe.34']}) for the datasets $D_{1}$ (SNIa+CC) and $D_{5}$ (SNIa+CC+BAO2025).
  • Figure 4: Theoretical prediction for the Hubble function $H(z)$ of the GUP and of the $\Lambda$CDM models. The cosmic chronometers are marked.