Is the Kaniadakis deformation of holographic dark energy detectable? A non-flat analysis with DESI DR2, cosmic chronometers and Pantheon+SH0ES
Abstract
Kaniadakis entropy deforms the horizon entropy through a single parameter K, and the holographic dark energy built on it (KHDE) reduces to the standard model as K→0. We ask whether current data can detect this deformation when spatial curvature is free and no cosmic-microwave-background calibration is assumed. Combining Pantheon+SH0ES supernovae, with the absolute magnitude fitted against the Cepheid calibrators, 32 cosmic-chronometer measurements of H(z) and DESI DR2 baryon acoustic oscillations with a free sound horizon, we find that non-flat KHDE fits the data as well as flat ΛCDM (Δχ2=−2.1 for three additional parameters) but leaves K unconstrained: the profile χ2 changes by only $0.47$ between K=0 and its best value, and the bound K<0.67 (95%) reflects the validity domain of the model rather than the data. Information criteria therefore prefer ΛCDM (ΔAIC=+3.9, ΔBIC=+20.2). The joint fit gives Ωk0=0.012±0.045, three times tighter than supernovae alone, H0=72.04±0.85 km s−1 Mpc−1 and rd=139.34±1.76 Mpc; chronometers and DESI alone prefer H0=68.17±1.93, 2.4σ below the supernova value. In the fitted model, acceleration begins at zt=0.66±0.03; a model-independent neural-network reconstruction of H(z) from the chronometers gives a present-day deceleration parameter q0=−0.46±0.14, consistent with the model. We also identify three analysis requirements which, if ignored, make the deformation numerically invisible, underestimate the H0 uncertainty fourfold, or spuriously reject the model.
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BibTeX
@misc{kumar2026kaniadakis,
title = {{Is the Kaniadakis deformation of holographic dark energy detectable? A non-flat analysis with DESI DR2, cosmic chronometers and Pantheon+SH0ES}},
author = {P. Suresh Kumar and Said Salim AL Kathiri},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.26883},
eprint = {2610.26883},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.26883},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Is the Kaniadakis deformation of holographic dark energy detectable? A non-flat analysis with DESI DR2, cosmic chronometers and Pantheon+SH0ES
AU - P. Suresh Kumar
AU - Said Salim AL Kathiri
PY - 2026
DA - 2026/10/09
PB - arXiv
DO - 10.48550/arxiv.2610.26883
UR - https://arxiv.org/abs/2610.26883
AB - Kaniadakis entropy deforms the horizon entropy through a single parameter K, and the holographic dark energy built on it (KHDE) reduces to the standard model as K→0. We ask whether current data can detect this deformation when spatial curvature is free and no cosmic-microwave-background calibration is assumed. Combining Pantheon+SH0ES supernovae, with the absolute magnitude fitted against the Cepheid calibrators, 32 cosmic-chronometer measurements of H(z) and DESI DR2 baryon acoustic oscillations with a free sound horizon, we find that non-flat KHDE fits the data as well as flat ΛCDM (Δχ^2=−2.1 for three additional parameters) but leaves K unconstrained: the profile χ^2 changes by only $0.47$ between K=0 and its best value, and the bound K<0.67 (95%) reflects the validity domain of the model rather than the data. Information criteria therefore prefer ΛCDM (ΔAIC=+3.9, ΔBIC=+20.2). The joint fit gives Ω_k0=0.012±0.045, three times tighter than supernovae alone, H_0=72.04±0.85 km s^−1 Mpc^−1 and r_d=139.34±1.76 Mpc; chronometers and DESI alone prefer H_0=68.17±1.93, 2.4σ below the supernova value. In the fitted model, acceleration begins at z_t=0.66±0.03; a model-independent neural-network reconstruction of H(z) from the chronometers gives a present-day deceleration parameter q_0=−0.46±0.14, consistent with the model. We also identify three analysis requirements which, if ignored, make the deformation numerically invisible, underestimate the H_0 uncertainty fourfold, or spuriously reject the model.
ER -