Constraining the dark energy models using baryon acoustic oscillations: An approach independent of H0 ⋅ rd

Open Access

Fig. 1.

Posterior distribution for for Ω_m, w₀, and w_a for different parametrizations of the wwaCDM model with the BAO and BAO_θ datasets to the left and to the right, respectively, and with the Pantheon data added to the bottom panels.

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