Marginalised probability distribution functions of H₀, Ω_m, Ω_Λ or Ω_DE, and w (from left to right) for different cosmological models (from top to bottom). Coloured lines show the one-dimensional posterior distributions obtained from various cosmological datasets: time-delay cosmography in MACS 1149 (r model) in blue; Planck (Planck Collaboration VI 2020) in orange; SH0ES (Riess et al. 2021) in green; Baryon acoustic oscillations (BAO) and redshift-space distortions (RSD; Alam et al. 2021) in red; the SN Pantheon sample (Scolnic et al. 2018) in purple; and H0LiCOW (Wong et al. 2020) in brown. Blue shaded regions represent the 68.3% (darker) and 95.4% (lighter) CL regions for time-delay cosmography in MACS 1149. For SH0ES, only the probability density distribution function of H₀ in a fΛCDM model is available and shown here. For BAORSD, we also included Gaussian priors on the values of ω_b and n_s (see the list of datasets in Sect. 3). For H0LiCOW, chains for the fΛCDM, oΛCDM and fwCDM models are available and here only the probability density distribution functions of H₀ and w are shown, since the adopted smaller prior on Ω_m causes a sharp edge in the posteriors of Ω_m and Ω_Λ or Ω_DE.