Table 4
Dependence of the best fitting values for the cosmological parameters Ωm and σ8 on the choice of other model parameters.
| Parameter |
|
|
ΔP | ΔΩm | Δσ8 |
|
|
|||||
| α sl | 2.2 | −1.3 | 10% | 22% | 13% |
| n 0 | −0.22 | −0.18 | 10% | −2.2% | −1.8% |
| scatter | 0.12 | −0.05 | 10% | 1.2% | −0.5% |
| scatter + ferr. | 0.16 | −0.07 | 10% | 1.6% | −0.7% |
|
|
|||||
| H 0 | −0.7 | 0.4 | 5% | −3.5% | 2% |
| Ωb | 0.15 | −0.07 | 10% | 1.5% | −0.7% |
| n s | −0.9 | 0.5 | 5% | −4.5% | 2.5% |
| Ωm + ΩΛ | ≤±0.11a) | ≤0.07 | 5% | ≤±0.5% | ≤0.35% |
| f mass | −0.3 | −0.28 | 10% | −3% | −3% |
| w | ≤0.02 | ≥ −0.02 | 10% | 0.15% | −0.19% |
Notes. First parameter set: slope αsl, normalization, n0, and scatter of the LX − M relation, and scatter combined with the flux error. Second parameter set: H0, Hubble constant, Ωb baryon density, ns slope of the primordial power spectrum, Ωm + ΩΛ − 1, degree of the deviation from a flat universe, fmass mass bias, and w, equation-of-state parameter for Dark Energy assumed to be constant. P heading the columns indicates the parameter of the row. ΔΩm and Δσ8 give the change in the resulting values for these two parameters upon a parameter variation, ΔP.
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