Table 2.
Parameters considered in the joint analysis of cluster counts and stacked weak lensing data.
Parameter | Description | Prior | Posterior |
---|---|---|---|
Ωm | Total matter density parameter | [0.09, 1] |
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σ8 | Amplitude of the matter power spectrum | [0.4, 1.5] |
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S8 ≡ σ8(Ωm/0.3)0.5 | Cluster normalisation parameter | – |
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α | Normalisation of the mass-observable scaling relation | [−2, 2] |
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β | Slope of the mass-observable scaling relation | [0, 5] |
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γ | Redshift evolution of the mass-observable scaling relation | [−4, 4] |
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σintr, 0 | Normalisation of σintr | [0.05, 1] |
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σintr, λ* | λ* evolution of σintr | [−5, 5] |
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Ωb | Baryon density parameter | 𝒩(0.0486, 0.0017) | – |
τ | Thomson scattering optical depth at re-ionisation | 𝒩(0.0544, 0.0365) | – |
ns | Primordial power spectrum spectral index | 𝒩(0.9649, 0.0210) | – |
h ≡ H0/(100 km s−1 Mpc−1) | Normalised Hubble constant | 𝒩(0.7, 0.1) | – |
s | Slope correction to the halo mass function | 𝒩(0.037, 0.014) | – |
q | Amplitude correction to the halo mass function | 𝒩(1.008, 0.019) | – |
δb | Fluctuation of the matter density due to super-survey modes | Gaussian (*) | – |
Notes. In the third column, the priors on the parameters are listed, and in particular a range represents a uniform prior, while 𝒩(μ, σ) stands for a Gaussian prior with mean μ and standard deviation σ. The Gaussian prior on δb is cosmology-dependent: both the mean and the standard deviation change at each MCMC step. In the fourth column, we show the median values of the 1D marginalised posteriors, along with the 16th and 84th percentiles. The posterior distributions of Ωb, τ, ns, h, s, q, and δb are not shown since these nuisance parameters are not constrained in our analysis.
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