Measuring the dark side (with weak lensing)

By Luca Amendola, Martin Kunz, D. Sapone. 2007

369 citations recorded by the source corpus.

We introduce a convenient parameterization of dark energy models that is general enough to include several modified gravity models and generalized forms of dark energy. In particular we take into account the linear perturbation growth factor, the anisotropic stress and the modified Poisson equation. We discuss the sensitivity of large-scale weak lensing surveys like the proposed DUNE satellite to these parameters (assuming systematic errors can be controlled). We find that a large-scale weak lensing tomographic survey is able to easily distinguish the Dvali–Gabadadze–Porrati model from ΛCDM and to determine the perturbation growth index to an absolute error of 0.02–0.04.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Oceanography

View Paper: https://www.semanticscholar.org/paper/c661f7e0463a2e463c1b80fecf542dbc8fd0cd67

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Citations in the corpus

CFHTLenS: testing the laws of gravity with tomographic weak lensing and redshift-space distortions (2012, methodology): “…are now modulated by the parameters Σ and µ Ψ(k, a) = [1 + µ(k, a)] ΨGR(k, a) , (4) [Ψ(k, a) + Φ(k, a)] = [1 + Σ(k, a)] [ΨGR(k, a) + ΦGR(k, a)] , (5) where we have adopted notation similar to that of Amendola et al. (2008), as used more recently by Zhao et al. (2010) and Song et al. (2011).”
Maximal freedom at minimum cost: linear large-scale structure in general modifications of gravity (2014, background): “Scalar perturbations dominate at linear scales and, in principle, all one needs to do is to relate the two scalar gravitational potentials to the matter distribution through some sort of parameterisation involving two functions of both scale and time [18–20].”
f(R) Theories (2010, background): “Since the evolution of matter perturbations and gravitational potentials is different from that of GR, the observations of weak lensing can provide us an important test for probing modified gravity on galactic scales (see [2, 527, 27, 595, 528, 548] for theoretical aspects and [546, 348, 322, 3, 629”
Modified Gravity and Cosmology (2011, methodology): “68We kept the original symbol GΦ here, although under our conventions it would be more accurately written as GΨ, as it plays the role of an effective gravitational constant for a modified Poisson equation for Ψ. • Amendola, Kunz and Sapone [41] modify the Poisson equation and the slip by considering”
Cosmological tests of modified gravity (2015, background): “For linear perturbations, one can parametrise the relation between the Newton potential to the density perturbations and the relation between the two metric perturbations [219, 220]”
Anisotropic dark energy: dynamics of the background and perturbations (2008, neutral): “weak lensing experiments [44]–[47].”
Effective field theory of dark energy: A review (2019, methodology): “A systematic investigation of possible DE/MG extensions to GR can be performed using the μ,Σ, η phenomenological approach [150, 151, 152, 153] reviewed in Section 3.”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “[54] find Euclid weak lensing constraints for a more general parameterization that includes evolution.”