Constraining viscous fluid models in $f(Q)$ gravity with data

We investigate the impact of bulk viscosity on the accelerating expansion and large-scale structure formation of a Universe in which the underlying gravitational interaction is described by $f(Q)$ gravity. Various paradigmatic choices of the $f(Q)$ gravity theory, including power-law, exponential, and logarithmic models, are considered. To test the cosmological viability of these $f(Q)$ gravity models, we use {the Baryon Acoustic Oscillations ($BAO$) measurements from the Dark Energy Spectroscopic Instrument (DESI) Survey, cosmic chronometers ($CC$) from Hubble measurements, the SNIa distance moduli measurements from the PantheonP + SH0ES, growth rate ($f$-data), and redshift-space distortions ($fσ_8$) datasets, the latter two once the linear cosmological perturbations, growth rate $f(z)$, and redshift-space distortion $fσ_8(z)$ are studied. Thus, we perform the combined analyses for: PantheonP + SH0ES, PantheonP + SH0ES + f, and PantheonP + SH0ES + $fσ_8$. We compute the best-fit values $Ω_m$, $H_0,\mathrm{(km/s/Mpc)}$, $r_d$, $M_{abs}$, $γ$, $σ_8$, $n$, $p$ and $Γ$ including the bulk viscosity coefficient $ζ$. Through a detailed statistical analysis, based on the Akaike Information Criterion (AIC) and Bayesian / Schwartz Information Criterion (BIC), a statistical comparison of the $f(Q)$ gravity models with $Λ$CDM is made. Among the three $f(Q)$ models, only the non-viscous $f(Q)$ power-law model yields robust parameter estimates and substantial observational support without any outright rejections. In contrast, both exponential and logarithmic $f(Q)$ models (with or without bulk viscosity) are rejected by multiple model selection criteria.

💡 Research Summary

This paper investigates the cosmological implications of bulk‑viscous fluids within the framework of $f(Q)$ gravity, where $Q$ denotes the non‑metricity scalar. Three representative functional forms of $f(Q)$ are examined: a power‑law model $F(Q)=\alpha Q^{n}$, an exponential model $F(Q)=\beta Q_{0}