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

2009/12/31 by Tatsuya Narikawa, Kazuhiro Yamamoto
Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Cosmology #Cosmology and Gravitation Theories #Dark energy #Galaxies: Formation, Evolution, Phenomena #Geometry #Mathematical physics #Physics #Quantum mechanics #Quintessence #Scalar (mathematics) #Scale (ratio) #Theoretical physics #astro-ph.CO

paper · pdf · doi:10.1103/physrevd.81.043528

published as Phys.Rev.D81:043528,2010; Erratum-ibid.D81:129903,2010 · 13 pages, 7 figures, typos corrected

openalex publication_date 2010/02/16 · arxiv created 2010/03/17 · arxiv updated 2014/11/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28

Abstract

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

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