Late-Time Alleviation of the Hubble Tension in CPL Cosmology with Massive Neutrinos via Bayesian Physics-Informed Neural Networks

arXiv:2601.00495 · astro-ph.CO, gr-qc · Submitted 2026-01-01 · Read on arXiv

astro-ph.CO, gr-qc

Submitted: 2026-01-01

Updated: 2026-09-13

Comments: 30 pages, 7figure

License: http://creativecommons.org/licenses/by/4.0/

The gist: We present a Bayesian analysis of the Hubble constant using Physics-Informed Neural Networks (PINNs), applied to the standard wCDM model and its dynamical extension via the

Terminology

Abstract

We present a Bayesian analysis of the Hubble constant using Physics-Informed Neural Networks (PINNs), applied to the standard wCDM model and its dynamical extension via the Chevallier--Polarski--Linder (CPL) parametrization, with and without a free summed neutrino mass Σm ν. Embedding the background Friedmann equation into a Bayesian PINN, we reconstruct H(z) in a data-driven, physically consistent way while propagating epistemic uncertainty. Combining Cosmic Chronometers, DESI DR2 BAO, and Pantheon+ supernovae with Planck 2018 CMB distance priors, we quantify the Hubble tension against Planck and SH0ES (R22). For wCDM, BAO-dominated combinations favor lower H 0, easing the Planck tension at the cost of a larger SH0ES discrepancy. Letting the equation of state evolve within CPL shifts H 0 upward and consistently favors a mildly quintessence-like w 0-1 with negative w a, pointing to a slowly evolving, non-phantom dark energy component. Adding a free Σm ν stabilizes H 0 between 69.7 and 71.6 km,s-1,Mpc-1, bounds Σm ν 0.16 -- 0.28 eV (2σ), and reduces the SH0ES tension below 1.8σ (down to 0.83σ) while the Planck tension persists at 1.6 -- 2.8σ. AIC and BIC both favor CPL+ Σm ν despite its extra parameters, arguing against overfitting. A full-CMB MCMC cross-check via Cobaya, including CMB lensing, reproduces the BPINN posteriors -- including the neutrino-mass bound -- within 1--2 σ at a fraction of the cost. A mildly evolving dark energy component combined with sub-eV neutrino masses thus substantially eases, though does not fully resolve, the Hubble tension, supporting Bayesian PINNs as an efficient, physically consistent tool for precision cosmology beyond Λ CDM.

Sources

Related papers