Cosmological tests of modified gravity: constraints on $F(R)$ theories from the galaxy clustering ratio

TL;DR

This paper demonstrates that the clustering ratio observable effectively constrains $F(R)$ modified gravity theories, with current data strongly supporting General Relativity and placing tight bounds on deviations.

Contribution

It introduces the clustering ratio as a sensitive cosmological probe of gravity and applies it to SDSS data to constrain $F(R)$ theories, providing competitive bounds.

Findings

GR fits galaxy clustering data up to z~0.6

Deviations from GR are constrained to be very small, |f_{R_0}| < 4.6e-5

Future surveys like Euclid will not significantly improve these bounds

Abstract

The clustering ratio $\eta$, a large-scale structure observable originally designed to constrain the shape of the power spectrum of matter density fluctuations, is shown to provide a sensitive probe of the nature of gravity in the cosmological regime. We apply this analysis to $F(R)$ theories of gravity using the luminous red galaxy (LRG) sample extracted from the spectroscopic Sloan Digital Sky Survey (SDSS) data release 7 and 10 catalogues. We find that General Relativity (GR), complemented with a Friedmann-Robertson-Walker (FRW) cosmological model with parameters fixed by the Planck satellite, describes extremely well the clustering of galaxies up to $z\sim 0.6$. On large cosmic scales, the absolute amplitude of deviations from GR, $|f_{R_0 }|$, is constrained to be smaller than $4.6 \times 10^{-5}$ at the $95\%$ confidence level. This bound makes cosmological probes of gravity almost competitive with the sensitivity of Solar System tests, although still one order of magnitude less effective than astrophysical tests. We also extrapolate our results to future large surveys like Euclid and show that the astrophysical bound will certainly remain out of reach for such a class of modified-gravity models that only differ from $\Lambda$CDM at low redshifts.