Constraints on the curvature of the Universe and dynamical dark energy from the full-shape and BAO data

We present limits on the parameters of the $\mathrm{o}\mathrm{\Lambda }\mathrm{CDM}$, $w_0\mathrm{CDM}$, and $w_0{w}_a\mathrm{CDM}$ models obtained from the joint analysis of the full-shape, baryon acoustic oscillations (BAO), big bang nucleosynthesis (BBN) and supernovae data. Our limits are fully independent of the data on the cosmic microwave background (CMB) anisotropies, but rival the CMB constraints in terms of parameter error bars. We find the spatial curvature consistent with a flat universe ${\mathrm{\Omega }}_k=-{0.043}_{-0.036}^{+0.036}$ (68% C.L.); the dark-energy equation of state parameter $w_0$ is measured to be $w_0=-{1.031}_{-0.048}^{+0.052}$ (68% C.L.), consistent with a cosmological constant. This conclusion also holds for the time-varying dark energy equation of state, for which we find $w_0=-{0.98}_{-0.11}^{+0.099}$ and $w_a=-{0.33}_{-0.48}^{+0.63}$ (both at 68% C.L.). The exclusion of the supernovae data from the analysis does not significantly weaken our bounds. This shows that using a single external BBN prior, the full-shape and BAO data can provide strong CMB-independent constraints on the nonminimal cosmological models.

Figure 1

Posterior distributions of the cosmological parameters of the $\mathrm{o}\mathrm{\Lambda }\mathrm{CDM}$ model.

Figure 2

Posterior distributions of the cosmological parameters of the $w_0\mathrm{CDM}$ model.

Figure 3

Posterior distributions of the cosmological parameters of the $w_0{w}_a\mathrm{CDM}$ model.

Figure 4

Posterior distributions of the cosmological parameters of the $\mathrm{\Lambda }\mathrm{CDM}$ model fitted to the PT Challenge mock data [83]. All parameters are normalized to represent the relative deviations from the fiducial values used in the $N$-body simulations.

Figure 5

Posterior distributions of the cosmological parameters of the $\mathrm{\Lambda }\mathrm{CDM}$ model fitted to the Nseries mock data for $k_{\max }=0.2h{\mathrm{Mpc}}^{-1}$.

Figure 6

Posterior distributions of the cosmological parameters of the $\mathrm{\Lambda }\mathrm{CDM}$ model fitted to the Nseries mock data for $k_{\max }=0.25h{\mathrm{Mpc}}^{-1}$.

Figure 7

Posterior distributions of the cosmological parameters of the $\mathrm{\Lambda }\mathrm{CDM}$ model inferred without and with the hexadecapole.

Figure 8

Posterior distributions of the cosmological parameters of the $w_0{w}_a\mathrm{CDM}$ model inferred without and with the hexadecapole.

Figure 9

Posterior distributions of the cosmological parameters of the $\mathrm{o}\mathrm{\Lambda }\mathrm{CDM}$ model.

Figure 10

Posterior distributions of the cosmological parameters of the $w_0\mathrm{CDM}$ model.

Figure 11

Posterior distributions of the cosmological parameters of the $w_0{w}_a\mathrm{CDM}$ model.