Table 2.
Model parameters and their priors grouped by the concordance model, extensions, and nuisance.
| Type | Parameter | Prior | Description |
|---|---|---|---|
| Flat ΛCDM | ωcdm | 𝒰(0.051, 0.255) | Cold dark matter density |
| ωb | 𝒰(0.019, 0.026) | Baryon density | |
| h | 𝒰(0.64, 0.82) | Reduced Hubble parameter | |
| ns | 𝒰(0.84, 1.1) | Spectral index of the primordial power spectrum | |
| S8 | 𝒰(0.5, 1.0) | Structure growth parameter | |
| ln 1010As | 𝒰(2.9, 3.2) | Matter power spectrum amplitude | |
| Extended | ∑mν[eV] | 𝒰(0, 3) | Sum of the neutrino masses |
| w0 | 𝒰(−3, 0) | Dark energy equation of state today | |
| wa | 𝒰(−5, 5) | Linear slope of the dark energy equation of state | |
| ΩK | 𝒰(−0.3, 0.3) | Spatial curvature density parameter | |
| Nuisance | log10TAGN | 𝒰(7.3, 8.3) | Baryon feedback parameter |
| AIA | 𝒩(5.74, CAIA, β) | Amplitude of intrinsic galaxy alignments for red galaxies | |
| β | 𝒩(0.44, CAIA, β) | Slope of the mass scaling of intrinsic galaxy alignments | |
| log10Mi | 𝒩(μ, CM) | Mean halo mass of early-type galaxies per tomographic bin i | |
| δz, i | 𝒩(μ, Cz) | Shift of the mean of the redshift distribution per tomographic bin i | |
Notes. The first two columns specify the types of the sampling parameters and the parameter names, respectively. The third column gives the priors used, with uniform priors denoted by their interval 𝒰, and Gaussian priors by 𝒩(μ, σ). The fourth column offers a brief description of each parameter. For more details on the chosen priors, see Wright et al. (2025b), Stölzner et al. (2025), Wright et al. (2025a). For nuisance parameters of the external probes, we use the fiducial priors from the respective analyses. When including any CMB data, we sample over log As instead of S8 and derive S8 instead. All constraints in Table 4 are, however, given in terms of S8 only. We tested that this choice does not introduce any information and yields the same cosmological constraints.
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