Tomography from the Next Generation of Cosmic Shear Experiments for Viable f(R) Models

Details Tomography from the Next Generation of Cosmic Shear Experiments for Viable f(R) Models Tomography from the Next Generation of Cosmic Shear Experiments for Viable f(R) Models

2011-04-14

arxiv.org/abs/1104.2740v2

JCAP07(2011)016

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

26 pages, 6 figures, 2 tables; tomographic and Bayesian analyses updated and modified according to reviewer's suggestions; ref

Scientific paper

10.1088/1475-7516/2011/07/016

We present the cosmic shear signal predicted by two viable cosmological models in the framework of modified-action f(R) theories. We use f(R) models where the current accelerated expansion of the Universe is a direct consequence of the modified gravitational Lagrangian rather than Dark Energy (DE), either in the form of vacuum energy/cosmological constant or of a dynamical scalar field (e.g. quintessence). We choose Starobinsky's (St) and Hu & Sawicki's (HS) f(R) models, which are carefully designed to pass the Solar System gravity tests. In order to further support - or rule out - f(R) theories as alternative candidates to the DE hypothesis, we exploit the power of weak gravitational lensing, specifically of cosmic shear. We calculate the tomographic shear matrix as it would be measured by the upcoming ESA Cosmic Vision Euclid satellite. We find that in the St model the cosmic shear signal is almost completely degenerate with LCDM, but it is easily distinguishable in the HS model. Moreover, we compute the corresponding Fisher matrix for both the St and HS models, thus obtaining forecasts for their cosmological parameters. Finally, we show that the Bayes factor for cosmic shear will definitely favour the HS model over LCDM if Euclid measures a value larger than ~0.02 for the extra HS parameter n_HS.

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