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The Observational Status of Galileon Gravity After Planck

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Structure Formation in Modified Gravity Cosmologies

Part of the book series: Springer Theses ((Springer Theses))

Abstract

To fully assess the observational viability of any cosmological model we must allow all of its parameters to vary within the observational constraints.

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Notes

  1. 1.

    The content in this chapter is based on the articles Barreira et al. “Parameter space in Galileon gravity models”, Phys. Rev. D 87, 103511, Published 15 May 2013, http://dx.doi.org/10.1103/PhysRevD.87.103511 (Ref. [1]) and Barreira et al. “The observational status of Galileon gravity after Planck”, Journal of Cosmology and Astroparticle Physics, Volume 2014, Published 27 August 2014, © IOP Publishing Ltd. Reproduced with permission. All rights reserved, http://dx.doi.org/10.1088/1475-7516/2014/08/059 (Ref. [2]).

  2. 2.

    This model is the best-fitting base Cubic Galilon model to the PLB dataset, but what is important in the discussion here is the impact of the initial conditions, regardless of which exact model parameters we consider.

  3. 3.

    In this chapter, we shall present results using the more recent CMB data from the Planck satellite, but for the purpose of discussing the scaling degeneracy here we can use these WMAP9 results.

  4. 4.

    In Ref. [43], without including the WiggleZ measurements in the BAO data, it was found that \(\chi ^2_{BAO} \sim 8\), for 3 dof.

  5. 5.

    In terms of the \(\Psi \) and \(\Phi \) potentials of the linearly perturbed FRW line element in the Newtonian gauge \(\mathrm{d}s^2 = \left( 1 + 2\Psi \right) \mathrm{d}t^2 - \left( 1 - 2\Phi \right) \mathrm{d}{x}^i\mathrm{d}{x}_i\), one has \(\phi = \left( \Psi + \Phi \right) /2\).

  6. 6.

    The q term is subdominant on small length scales (large k) and for matter \(\Pi = 0\). In this case, one then recovers the standard Poisson equation \(-k^2\phi = 4\pi G a^2\chi \).

  7. 7.

    To first approximation, we assume also that all of the matter components (baryons, CDM and massive neutrinos) contribute equally to \(\delta \).

  8. 8.

    We note that this observational tension arises when one considers the background evolution of the Galileon field when making a prediction for the Solar System. If \(\dot{\bar{\varphi }} = 0\), then the tension goes away. In Chap. 6, we shall discuss this more indepth when we encounter a similar tension for Nonlocal gravity.

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  1. Max Planck Institute for Astrophysics, Garching, Germany

    Alexandre Barreira

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Barreira, A. (2016). The Observational Status of Galileon Gravity After Planck. In: Structure Formation in Modified Gravity Cosmologies. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-33696-1_3

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