https://doi.org/10.1140/epjc/s10052-016-3997-9
Regular Article - Theoretical Physics
Breaking CMB degeneracy in dark energy through LSS
School of Physics, Korea Institute for Advanced Study, Heogiro 85, Seoul, 130-722, Korea
* e-mail: skylee@kias.re.kr
Received:
23
September
2015
Accepted:
2
March
2016
Published online:
19
March
2016
The cosmic microwave background (CMB) and large-scale structure (LSS) are complementary probes in the investigatation of the early and late time Universe. After the current accomplishment of the high accuracies of CMB measurements, accompanying precision cosmology from LSS data is emphasized. We investigate the dynamical dark energy (DE) models which can produce the same CMB angular power spectra as that of the 
CDM model with less than a sub-percent level accuracy. If one adopts the dynamical DE models using the so-called Chevallier–Polarski–Linder (CPL) parametrization, 
, then one obtains models 
named M8, M9, M11, and M12, respectively. The differences of the growth rate, f, which is related to the redshift-space distortions (RSD) between different DE models and the CDM model are about 0.2 % only at z = 0. The difference of f between M8 (M9, M11, M12) and the CDM model becomes maximum at 
with 
%. This is a scale-independent quantity. One can investigate the one-loop correction of the matter power spectrum of each model using the standard perturbation theory in order to probe the scale-dependent quantity in the quasi-linear regime (i.e. 
). The differences in the matter power spectra including the one-loop correction between M8 (M9, M11, M12) and the CDM model for the 
scale are 1.8 (0.9, 1.2, 3.0) % at 
, 3.0 (1.6, 1.9, 4.2) % at 
, and 3.2 (1.7, 2.0, 4.5) % at 
. The larger departure from 
of 
, the larger the difference in the power spectrum. Thus, one should use both the RSD and the quasi-linear observable in order to discriminate a viable DE model among a slew of the models which are degenerate in CMB. Also we obtain the lower limit on 
from the CMB acoustic peaks and this will provide a useful limitation on phantom models.
© The Author(s), 2016
