New Tsallis holographic dark energy with the Granda-Oliveros cutoff in a non-flat universe: curvature tracking and DESI DR2 constraints
Abstract
Holographic dark energy ties the dark-energy density to an infrared length. We study new Tsallis holographic dark energy (NTHDE), built on the exponential Tsallis entropy, with the local Granda-Oliveros (GO) cutoff L−2=αH2+γḢ in a spatially curved universe. Writing the background as an autonomous system for (Ωd,u,Ωk), we obtain four exact results. (i) In the closed-form solution without the Tsallis deformation, the dark energy splits into a matter-like and a curvature-like part. (ii) Because the GO cutoff lacks the term k/a2 of the Ricci scalar, the coefficient of (1+z)2 in H2/H02 is RkΩk0 with Rk=(1−α+γ)−1>1, while distances and the Clarkson-Bassett-Lu test return Ωk0; the Ricci completion restores Rk=1. (iii) Big-bang nucleosynthesis locks the matter-era dark-energy fraction to 1/(1+3|wGO|), where wGO is the equation of state of the GO mode. (iv) The finite-time fold singularity of the flat model survives curvature. Against Pantheon+SH0ES supernovae, 32 cosmic chronometers and DESI DR2 BAO, curved GO-NTHDE gives Ωk0=−0.001+0.041−0.043, consistent with flatness, and Δχ2=−2.82 relative to flat ΛCDM, but the Bayesian evidence prefers flat ΛCDM (ln B=−2.66±0.24), and allowing curvature costs ln B=−1.39±0.25. The data cannot yet measure Rk: the GO and Ricci cutoffs fit equally well (ln B=+0.28±0.26). With Union3 supernovae the model is on a par with ΛCDM (ln B=+0.53). A fraction 0.91 of the posterior reaches the finite-time fold.
Related
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BibTeX
@misc{sharma2026tsallis,
title = {{New Tsallis holographic dark energy with the Granda-Oliveros cutoff in a non-flat universe: curvature tracking and DESI DR2 constraints}},
author = {Umesh Kumar Sharma and Pankaj and Bramha Dutta Pandey and P. Suresh Kumar},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.00194},
eprint = {2610.00194},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.00194},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - New Tsallis holographic dark energy with the Granda-Oliveros cutoff in a non-flat universe: curvature tracking and DESI DR2 constraints
AU - Umesh Kumar Sharma
AU - Pankaj
AU - Bramha Dutta Pandey
AU - P. Suresh Kumar
PY - 2026
DA - 2026/10/03
PB - arXiv
DO - 10.48550/arxiv.2610.00194
UR - https://arxiv.org/abs/2610.00194
AB - Holographic dark energy ties the dark-energy density to an infrared length. We study new Tsallis holographic dark energy (NTHDE), built on the exponential Tsallis entropy, with the local Granda-Oliveros (GO) cutoff L^−2=αH^2+γḢ in a spatially curved universe. Writing the background as an autonomous system for (Ω_d,u,Ω_k), we obtain four exact results. (i) In the closed-form solution without the Tsallis deformation, the dark energy splits into a matter-like and a curvature-like part. (ii) Because the GO cutoff lacks the term k/a^2 of the Ricci scalar, the coefficient of (1+z)^2 in H^2/H_0^2 is R_kΩ_k0 with R_k=(1−α+γ)^−1>1, while distances and the Clarkson-Bassett-Lu test return Ω_k0; the Ricci completion restores R_k=1. (iii) Big-bang nucleosynthesis locks the matter-era dark-energy fraction to 1/(1+3|w_GO|), where w_GO is the equation of state of the GO mode. (iv) The finite-time fold singularity of the flat model survives curvature. Against Pantheon+SH0ES supernovae, 32 cosmic chronometers and DESI DR2 BAO, curved GO-NTHDE gives Ω_k0=−0.001^+0.041_−0.043, consistent with flatness, and Δχ^2=−2.82 relative to flat ΛCDM, but the Bayesian evidence prefers flat ΛCDM (ln B=−2.66±0.24), and allowing curvature costs ln B=−1.39±0.25. The data cannot yet measure R_k: the GO and Ricci cutoffs fit equally well (ln B=+0.28±0.26). With Union3 supernovae the model is on a par with ΛCDM (ln B=+0.53). A fraction 0.91 of the posterior reaches the finite-time fold.
ER -