Cosmological implications of different baryon acoustic oscillation data

Abstract

In this work, we explore the cosmological implications of different baryon acoustic oscillation (BAO) data, including the BAO data extracted by using the spherically averaged one-dimensional galaxy clustering (GC) statistics (hereafter BAO1) and the BAO data obtained by using the anisotropic two-dimensional GC statistics (hereafter BAO2). To make a comparison, we also take into account the case without BAO data (hereafter NO BAO). Firstly, making use of these BAO data, as well as the SNLS3 type Ia supernovae sample and the Planck distance priors data, we give the cosmological constraints of the ΛCDM, the wCDM, and the Chevallier-Polarski-Linder (CPL) model. Then, we discuss the impacts of different BAO data on cosmological consquences, including its effects on parameter space, equation of state (EoS), figure of merit (FoM), decelerationacceleration transition redshift, Hubble parameter H(z), deceleration parameter q(z), statefinder hierarchy S 4 (z) and cosmic age t(z). We find that: (1) NO BAO data always give a smallest fractional matter density Ωm0, a largest fractional curvature density Ω k0 and a largest Hubble constant h; in contrast, BAO1 data always give a largest Ωm0, a smallest Ω k0 and a smallest h. (2) For the wCDM and the CPL model, NO BAO data always give a largest EoS w; in contrast, BAO2 data always give a smallest w. (3) Compared with the case of BAO1, BAO2 data always give a slightly larger FoM, and thus can give a cosmological constraint with a slightly better accuracy. (4) The impacts of different BAO data on the cosmic evolution and the comic age are very small, and can not be distinguished by using various dark energy diagnosis and the cosmic age data.PACS numbers: 98.80.Es, 95.36.+x

Diagnosing holographic type dark energy models with the Statefinder hierarchy, composite null diagnostic and w-w′ pair

“…In 2004, Li proposed the so-called holographic dark energy (HDE) model [26], which is the first DE model inspired by the HP. This model is in very good agreement with current observational data [27][28][29][30][31][32][33] and has drawn a lot of attention in recent 10 years [34][35][36][37][38][39][40][41]. In addition to HDE, some other HP-inspired DE models have also been proposed, such as the new agegraphic dark energy (NADE) model [42] and the Ricci dark energy (RDE) model [43].…”

Holographic dark energy

“…In [430], Zhang et al further diagnosed these four HP-inspired DE models with statefinder hierarchy S = A4 + 3(1 + q), where A3 and A4 are given in Eq.63. For more studies about statefinder hierarchy, see [432,433]. 18 The fractional growth parameter is defined as [434,435] figure, one can also clearly see that, there are significant differences among the evolution of S (1) 4 ( ) given by the four HP-inspired DE models.…”

“…From this 17 The statefinder hierarchy satisfy [431] S = A4 + 3(1 + q), where A3 and A4 are given in Eq.63. For more studies about statefinder hierarchy, see [432,433]. 18 The fractional growth parameter is defined as [434,435] ≡ f model (z)/fΛCDM (z), where f (z) = d ln δ/d ln a describes the growth rate of the linear density perturbation.…”

A low Hubble constant from galaxy distribution observations

“…3 The Robustness of baryon acoustic oscillations constraints in models beyond the flat ΛCDM model have been verified and discussed in details, for instance, in the works of [18] and [19]. 1.…”