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We investigate the linear growth rate of cosmological matter densityperturbations of a viable f(R) model both numerically and analytically. We findthat the growth rate in the scalar-tensor regime can be characterized by asimple analytic formula. We also investigate a prospect of constraining theCompton wavelength scale of the f(R) model with a future weak lensing survey.

Characterizing the linear growth rate of cosmological density perturbations in an f(R) model