f(Q,T) Gravity with Barrow Holographic Dark Energy and Massive Neutrinos: DESI DR2 Constraints and Implications for the Hubble Tension
Abstract
We study a modification of symmetric teleparallel gravity in which the function f(Q,T) is linear in the non-metricity scalar Q and the trace T of the energy-momentum tensor, combined with a Barrow holographic dark energy (BHDE) density built from the Granda-Oliveros infrared cutoff. The resulting background equations are solved in a modified version of \texttt{hi\_class} and constrained with Pantheon+ supernovae, 32 cosmic chronometer H(z) points, DESI DR2 baryon acoustic oscillations, and Planck 2018 CMB distance priors, sampled with MontePython. Two versions of the model are considered, one with the neutrino sector held massless and one with the sum of neutrino masses Σmν left free. Across five data combinations, H0 falls between 67.5 and 72.3 km s−1 Mpc−1, closer to the Planck value when cosmic chronometers dominate the fit and closer to the SH0ES value when Pantheon+ is included; adding Σmν as a free parameter raises H0 in four of the five combinations, by amounts ranging from a few hundredths of a km s−1 Mpc−1 up to about 1.5 km s−1 Mpc−1, while the CMB-only combination shifts slightly the other way, and the fit uncertainties loosen throughout. The 95\% upper bound on Σmν ranges from 0.13 to 0.22 eV depending on the data combination, comparable to standard ΛCDM constraints. Comparison with ΛCDM through the Akaike and Bayesian Information Criteria gives mixed results: the extended model is favored once Pantheon+ is included, particularly with massive neutrinos, but is disfavored for CMB-only and CMB+BAO fits, where the improvement in χ2 does not offset the larger parameter count. The Barrow exponent Δ stays below 0.005 throughout, and the Granda-Oliveros parameters λ and γ remain near 1 and 0.5 across all combinations.
Related
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BibTeX
@misc{tohidi2026gravity,
title = {{$f(Q,T)$ Gravity with Barrow Holographic Dark Energy and Massive Neutrinos: DESI DR2 Constraints and Implications for the Hubble Tension}},
author = {Ameneh Tohidi and Amin Salehi and Muhammad Yarahmadi},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.23957},
eprint = {2610.23957},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.23957},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - f(Q,T) Gravity with Barrow Holographic Dark Energy and Massive Neutrinos: DESI DR2 Constraints and Implications for the Hubble Tension
AU - Ameneh Tohidi
AU - Amin Salehi
AU - Muhammad Yarahmadi
PY - 2026
DA - 2026/10/09
PB - arXiv
DO - 10.48550/arxiv.2610.23957
UR - https://arxiv.org/abs/2610.23957
AB - We study a modification of symmetric teleparallel gravity in which the function f(Q,T) is linear in the non-metricity scalar Q and the trace T of the energy-momentum tensor, combined with a Barrow holographic dark energy (BHDE) density built from the Granda-Oliveros infrared cutoff. The resulting background equations are solved in a modified version of \texttt{hi\_class} and constrained with Pantheon+ supernovae, 32 cosmic chronometer H(z) points, DESI DR2 baryon acoustic oscillations, and Planck 2018 CMB distance priors, sampled with MontePython. Two versions of the model are considered, one with the neutrino sector held massless and one with the sum of neutrino masses Σm_ν left free. Across five data combinations, H_0 falls between 67.5 and 72.3 km s^−1 Mpc^−1, closer to the Planck value when cosmic chronometers dominate the fit and closer to the SH0ES value when Pantheon+ is included; adding Σm_ν as a free parameter raises H_0 in four of the five combinations, by amounts ranging from a few hundredths of a km s^−1 Mpc^−1 up to about 1.5 km s^−1 Mpc^−1, while the CMB-only combination shifts slightly the other way, and the fit uncertainties loosen throughout. The 95\% upper bound on Σm_ν ranges from 0.13 to 0.22 eV depending on the data combination, comparable to standard ΛCDM constraints. Comparison with ΛCDM through the Akaike and Bayesian Information Criteria gives mixed results: the extended model is favored once Pantheon+ is included, particularly with massive neutrinos, but is disfavored for CMB-only and CMB+BAO fits, where the improvement in χ^2 does not offset the larger parameter count. The Barrow exponent Δ stays below 0.005 throughout, and the Granda-Oliveros parameters λ and γ remain near 1 and 0.5 across all combinations.
ER -