Table 1.
Definition of the parameters and priors used in the analysis for all the different parameterizations and models considered.
| Cosmological parameters | Priors | |
|---|---|---|
| Ωm | Mean matter density at present time | 𝒰(0.05, 0.95) |
| + θ* priors (see Appendix F) | ||
| log10As | Amplitude of the primordial power spectrum | 𝒰(−10, −8) |
| H0 | Hubble expansion rate (km s−1 Mpc−1) at present time | 𝒩(70, 52) |
| Ωb | Mean baryon density at present time | 𝒰(0.046, 0.052) |
| ns | Spectra index of the primordial power spectrum | 𝒰(0.92, 1.0) |
| w | Dark energy equation of state. Fixed to −1 in ΛCDM | 𝒰(−2.5, −0.33) |
| Power spectrum suppression | Priors | |
| γ | Cosmic linear growth index | 𝒰(0.05, 0.95) |
| β | Power spectrum reduction parameter | 𝒰(−5, 5) |
| p | Power spectrum reduction index | Fixed to 1 |
| X-ray scaling relation | Priors | |
| AX | Normalization of the M − CR scaling relation | 𝒰(0.01, 16) |
| BX | Mass slope of the M − CR scaling relation | 𝒰(0.1, 5) |
| DX | Luminosity distance evolution of the M − CR scaling relation | Fixed to −2 |
| EX | Scale factor evolution of the M − CR scaling relation | Fixed to 2 |
| FX | Redshift evolution of the mass slope of the M − CR scaling relation | 𝒰(−10, 10) |
| GX | Redshift evolution of the normalization of the M − CR scaling relation | 𝒰(−10, 10) |
| σX | Intrinsic scatter of the M − CR scaling relation | 𝒰(0.01, 8) |
| Richness mass calibration | Priors | |
| lnAλ | Normalization of the M − λ scaling relation | 𝒰(1, 6) |
| Bλ | Mass slope of the M − λ scaling relation | 𝒰(0, 2) |
| Cλ | Redshift evolution of the normalization of the M − λ scaling relation | 𝒰(−10, 10) |
| Dλ | Redshift evolution of the mass slope of the M − λ scaling relation | 𝒰(−10, 10) |
| σλ | Intrinsic scatter of the M − λ scaling relation | 𝒰(0.01, 5) |
| ρλ, CR | Intrinsic correlation between richness and count rate | 𝒰(−0.9, 0.9) |
Notes. 𝒰(min, max) indicates a uniform distribution between ‘min’ and ‘max’ and 𝒩(μ, σ2) indicates a normal distribution centered on μ and with standard deviation σ. We only represent the parameters for which differences exist between this work and G24. We do not represent the additional parameters related to the uncertainties on the weak lensing mass calibration, the redshift uncertainties, and the contamination modeling. See G24 for the details on these parameters.
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