Structure growth in $f(Q)$ cosmology

Abstract

We take into account redshift-space distortion measurements to investigate the growth of cosmological large-scale structures within the framework of modified symmetric teleparallel $f(Q)$ gravity. After comparing the predictions of the $f(Q)$-gravity expansion history with OHD and SNIa Pantheon+ sample datasets and constraining the pertinent cosmological parameters ${\Omega }_m$ and $H_0$, together with the exponent $n$ for $f(Q)$ power-law models, we derive the full system of equations governing linear cosmological perturbations to study matter fluctuations using the $1+3$ covariant formalism when applied to $f(Q)$ gravity. Thus, we resort to both the usual redshift-space distortion data $f{\sigma }_8$ and some recent separate measurements of the growth rate $f$ and the amplitude of matter fluctuations ${\sigma }_8$ from the VIPERS and SDSS collaborations to find the best-fit cosmological parameters ${\Omega }_m$, ${\sigma }_8$ and $n$. We also apply a collective analysis of such growth-structure data together with the aforementioned cosmic expansion measurements, to restrict these parameters through Monte Carlo Markov Chain simulations. determining the statistical significance for the best-fit parameter values through the AIC and BIC Bayesian selection criteria.

arXiv comment7 Figures, 6 Tables, 22 pages. Accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS)

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