Cosmological Tests of Gravity

Ferreira, Pedro G.

doi:10.1146/annurev-astro-091918-104423

Cited by 180 publications

(132 citation statements)

References 176 publications

(155 reference statements)

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“…We notice that the approximation of static kernels, usually taken in ΛCDM and exact for EdS, corresponds to Γ f n Γ n , (ΛCDM), (A. 13) and therefore, the functions presented in the rest of this appendix can be recasted in their well-known, ΛCDM counterparts by omitting the "f " labels.…”

Section: A1 Lpt Kernelsmentioning

confidence: 99%

An accurate perturbative approach to redshift space clustering of biased tracers in modified gravity

Valogiannis

Bean

Avilés

2020

J. Cosmol. Astropart. Phys.

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We extend the scale-dependent Gaussian Streaming Model (GSM) to produce analytical predictions for the anisotropic redshift-space correlation function for biased tracers in modified gravity models.Employing the Convolution Lagrangian Perturbation Theory (CLPT) re-summation scheme, with a local Lagrangian bias schema provided by the peak-background split formalism, we predict the necessary ingredients that enter the GSM, the real-space halo pairwise velocity and the pairwise velocity dispersion. We apply our method on two widely-considered modified gravity models, the chameleon-screened f (R) Hu-Sawicki model and the nDGP Vainshtein model and compare our predictions against state-of-the-art N-body simulations for these models.We demonstrate that the GSM approach to predict the monopole and the quadrupole of the redshift-space correlation function for halos, gives very good agreement with the simulation data, for a wide range of screening mechanisms, levels of screening and halo masses at z = 0.5 and z = 1. Our work shows the applicability of the GSM, for cosmologies beyond GR, demonstrating that it can serve as a powerful predictive tool for the next stage of cosmological surveys like DESI, Euclid, LSST and WFIRST. arXiv:1909.05261v1 [astro-ph.CO]

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Section: A1 Lpt Kernelsmentioning

confidence: 99%

An accurate perturbative approach to redshift space clustering of biased tracers in modified gravity

Valogiannis

Bean

Avilés

2020

J. Cosmol. Astropart. Phys.

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“…Effectively, p ≫ 1 freezes the dynamics of σ. This is not dissimilar to screening mechanisms in modified gravity where Vainshtein screening (or k-mouflage) works by decoupling the field through a large kinetic term [13][14][15].…”

Section: Figmentioning

confidence: 99%

Pole dark energy

Linder

2020

Phys. Rev. D

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Theories with a pole in the kinetic term have been used to great effect in studying inflation, owing to their quantum stability and attractor properties. We explore the use of such pole kinetic terms in dark energy theories, finding an interesting link between thawing and freezing models, and the possibility of enhanced plateaus with "superattractor"-like behavior. We assess the observational viability of pole dark energy, showing that simple models can give dark energy equation of state evolution with w(z) < −0.9 even for potentials that could not normally achieve this easily. The kinetic term pole also offers an interesting perspective with respect to the swampland criteria for such observationally viable dark energy models.

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“…Although the latter gives a precise description of the Universe, it is known that it still contains a number of unresolved problems [1]. These lead researchers to look for alternatives in the forms of an additional dark fluid, namely dark energy (DE) or modifying the gravitational law at cosmological scales, for example by including additional degrees of freedom (dofs), defining the so called modified gravity theories (MG) [1][2][3][4][5][6][7][8][9][10]. One of the most studied proposal of MG is the Horndeski theory (or Galileon theory) [11,12], characterized by the presence of four free functions, namely [G 2 , G 3 , G 4 , G 5 ][φ, X], where φ is the extra scalar field, whose dynamics is settled by second order equations of motion, and X = ∂ µ φ∂ µ φ.…”

Section: Introductionmentioning

confidence: 99%

Phenomenology of the generalized cubic covariant Galileon model and cosmological bounds

et al. 2020

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We investigate the generalized cubic covariant Galileon model, a kinetically driven dark energy model within the Horndeski class of theories. The model extends the cubic covariant Galileon by including power laws of the field derivatives in the K-essence and cubic terms which still allow for tracker solutions. We study the shape of the viable parameter space by enforcing stability conditions which include the absence of ghost, gradient and tachyon instabilities and the avoidance of strong coupling at early time. We study here the relevant effects of the modifications induced by the model on some cosmological observables such as the cosmic microwave background (CMB), the lensing potential auto-correlation and the matter power spectrum. For this goal, we perform parameter estimation using data of CMB temperature and polarization, baryonic acoustic oscillations (BAO), redshift-space distortions (RSD), supernovae type Ia (SNIa) and Cepheids. Data analysis with CMB alone finds that the today's Hubble parameter H 0 is consistent with its determination from Cepheids at 1σ, resolving the famous tension of the cosmological standard models. The joint analysis of CMB, BAO, RSD and SNIa sets a lower bound for the sum of neutrino masses which is Σm ν > 0.11 eV at 1σ, in addition to the usual upper limit. The model selection analysis based on the effective χ 2 eff and Deviance Information Criterion is not able to clearly identify the statistically favored model between ΛCDM and the generalized cubic covariant Galileon, from which we conclude that the latter model deserves further studies.

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Cosmological Tests of Gravity

Cited by 180 publications

References 176 publications

An accurate perturbative approach to redshift space clustering of biased tracers in modified gravity

An accurate perturbative approach to redshift space clustering of biased tracers in modified gravity

Pole dark energy

Phenomenology of the generalized cubic covariant Galileon model and cosmological bounds

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