Cosmological perturbations and observational constraints on nonlocal massive gravity

Abstract

Nonlocal massive gravity can provide an interesting explanation for the late-time cosmic acceleration, with a dark energy equation of state $w_{\mathrm{DE}}$ smaller than $-1$ in the past. We derive the equations of linear cosmological perturbations to confront such models with the observations of large-scale structures. The effective gravitational coupling to nonrelativistic matter associated with galaxy clusterings is close to Newton's gravitational constant $G$ for a mass scale $m$ slightly smaller than today's Hubble parameter $H_0$. Taking into account the background expansion history as well as the evolution of matter perturbations ${\delta }_m$, we test for these models with Type Ia Supernovae (SnIa) from Union 2.1, the cosmic microwave background (CMB) measurements from Planck, a collection of baryon acoustic oscillations (BAO), and the growth rate data of ${\delta }_m$. Using a higher value of $H_0$ derived from its direct measurement ($H_0\gtrsim 70$ km s${}^{-1}$ Mpc${}^{-1}$) the data strongly support the nonlocal massive gravity model ($-1.1\lesssim w_{\mathrm{DE}}\lesssim -1.04$ in the past) over the $\Lambda$CDM model ($w_{\mathrm{DE}}=-1$), whereas for a lower prior (67 km s${}^{-1}$ Mpc${}^{-1}$ $\lesssim$ $H_0\lesssim 70$ km s${}^{-1}$ Mpc${}^{-1}$) the two models are statistically comparable.

16 pages, 6 figures, changes match published version

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