Cosmological Bounds on the Generalized Uncertainty Principle from the CMB
Abstract
We constrain the deformation parameter β of the Generalized Uncertainty Principle with cosmological observations. A quadratic deformation of the Heisenberg uncertainty principle modifies the Friedmann equations of ΛCDM and gives rise to a phenomenological dynamical dark energy with a single free parameter, β. To avoid a singular behaviour for the effective dark energy equation of state parameter, we restrict the prior to non-negative values of β. Using Planck 2018 CMB temperature and polarization data together with DESI DR2 BAO and Pantheon+SH0ES supernovae, we find the upper limit β<0.00728 at 68% confidence interval. The resulting cosmological model fits the data slightly better than ΛCDM, providing smaller value for the $χ_{min}^{2}% $, such that the Akaike Information Criterion to suggest statistical equivalency between the two models, although the Bayesian evidence favours the ΛCDM. Finally, the quadratic Generalized Uncertainty Principle does not alleviate the H0 tension, it reduces the tension to 4.8σ, that is, due to the small correlation between the H0−β parameters.
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BibTeX
@misc{paliathanasis2026cosmological,
title = {{Cosmological Bounds on the Generalized Uncertainty Principle from the CMB}},
author = {Andronikos Paliathanasis},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.28664},
eprint = {2610.28664},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.28664},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Cosmological Bounds on the Generalized Uncertainty Principle from the CMB
AU - Andronikos Paliathanasis
PY - 2026
DA - 2026/10/14
PB - arXiv
DO - 10.48550/arxiv.2610.28664
UR - https://arxiv.org/abs/2610.28664
AB - We constrain the deformation parameter β of the Generalized Uncertainty Principle with cosmological observations. A quadratic deformation of the Heisenberg uncertainty principle modifies the Friedmann equations of ΛCDM and gives rise to a phenomenological dynamical dark energy with a single free parameter, β. To avoid a singular behaviour for the effective dark energy equation of state parameter, we restrict the prior to non-negative values of β. Using Planck 2018 CMB temperature and polarization data together with DESI DR2 BAO and Pantheon+SH0ES supernovae, we find the upper limit β<0.00728 at 68% confidence interval. The resulting cosmological model fits the data slightly better than ΛCDM, providing smaller value for the $χ_{min}^{2}% $, such that the Akaike Information Criterion to suggest statistical equivalency between the two models, although the Bayesian evidence favours the ΛCDM. Finally, the quadratic Generalized Uncertainty Principle does not alleviate the H_0 tension, it reduces the tension to 4.8σ, that is, due to the small correlation between the H_0−β parameters.
ER -