Observational constraints on Galileon cosmology

By S. Nesseris, Antonio de Felice, S. Tsujikawa. 2010

134 citations recorded by the source corpus.

We study the cosmology of a covariant Galileon field φ with five covariant Lagrangians and confront this theory with the most recent cosmological probes: the type Ia supernovae data (Constitution and Union2 sets), cosmic microwave background (WMAP7), and the baryon acoustic oscillations (SDSS7). In the Galileon cosmology with a late-time de Sitter attractor, there is a tracker that attracts solutions with different initial conditions to a common trajectory. Including the cosmic curvature K, we place observational constraints on two distinct cases: (i) the tracker, and (ii) the generic solutions to the equations of motion. We find that the tracker solution can be consistent with the individual observational data, but it is disfavored by the combined data analysis. The generic solutions fare quite well when a nonzero curvature parameter Ω (0) K is taken into account, but the Akaike and Bayesian information criteria show that they are not particularly favored over the ACDM model.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/babacb4bd4b6ced4deade26b2d364f78715e5486

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Citations in the corpus

The imperfect fluid behind kinetic gravity braiding (2011, background): “Nonetheless, these theories have been named galileon theories and a significant body of work has already been carried out analysing their impact not only on cosmological solutions [28–45], but also in other circumstances [46–55].”
Modified Gravity and Cosmology (2011, background): “Schmidt then proceeds to calculate the halo mass function, and shows that the abundance of massive halos in self-accelerating DGP is much smaller than in CDM models.”
Cosmology in generalized Proca theories (2016, background): “Unfortunately, this case is in tension with the combined observational constraints of SNIa, CMB, and BAO due to the large deviation of wDE from −1 before the onset of cosmic acceleration [95].”