Cosmological constraints and phenomenology of a beyond-Horndeski model
  We study observational constraints on a specific dark energy model in the
framework of Gleyzes-Langlois-Piazza-Vernizzi theories, which extends the
Galileon ghost condensate (GGC) to the domain of beyond Horndeski theories. In
this model, we show that the Planck cosmic microwave background (CMB) data,
combined with datasets of baryon acoustic oscillations, supernovae type Ia, and
redshift-space distortions, give the tight upper bound $|\alpha_{\rm H}^{(0)}|
\le {\cal O}(10^{-6})$ on today's beyond-Horndeski (BH) parameter $\alpha_{\rm
H}$. This is mostly attributed to the shift of CMB acoustic peaks induced by
the early-time changes of cosmological background and perturbations arising
from the dominance of $\alpha_{\rm H}$ in the dark energy density. In
comparison to the $\Lambda$-cold-dark-matter ($\Lambda$CDM) model, our BH model
suppresses the large-scale integrated-Sachs-Wolfe (ISW) tail of CMB temperature
anisotropies due to the existence of cubic Galileons, and it modifies the
small-scale CMB power spectrum because of the different background evolution.
We find that the BH model considered fits the data better than $\Lambda$CDM
according to the $\chi^2$ statistics, yet the deviance information criterion
(DIC) slightly favors the latter. Given the fact that our BH model with
$\alpha_{\rm H}=0$ (i.e., the GGC model) is favored over $\Lambda$CDM even by
the DIC, there are no particular signatures for the departure from Horndeski
theories in current observations.
