Cosmological constraints from the observed angular cross-power spectrum between Sunyaev-Zel’dovich and X-ray surveys

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Volume 576 (April 2015)

A&A, 576 (2015) A90

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Table 2

Best-fitting values for Σ₈ for different data subsets.


Dataset	Model	⟨ Σ₈ ⟩	Σ_8,max		68% interval	ΔSyst


X-rays × 70–545 GHz	Eq. (18)	0.804	0.805	0.006	0.800–0.809	0.001	1.22

X-rays × 70 GHz	Eq. (17)	0.782	0.784	0.015	0.770–0.798	0.020	1.51
X-rays × 100 GHz	Eq. (17)	0.798	0.799	0.007	0.793–0.805	0.010	0.94
X-rays × 143 GHz	Eq. (17)	0.799	0.799	0.006	0.794–0.804	0.010	1.24
X-rays × 353 GHz	Eq. (17)	0.815	0.816	0.008	0.809–0.823	0.015	0.61

X-rays × 70 GHz	Eq. (18)	0.791	0.790	0.020	0.771–0.809	0.001	1.51
X-rays × 100 GHz	Eq. (18)	0.815	0.816	0.010	0.807–0.824	0.001	0.85
X-rays × 143 GHz	Eq. (18)	0.806	0.806	0.007	0.800–0.812	0.001	1.20
X-rays × 353 GHz	Eq. (18)	0.808	0.809	0.008	0.801–0.816	0.001	0.61
X-rays × 545 GHz	Eq. (18)	0.803	0.808	0.018	0.790–0.822	0.001	1.35

X-rays ×y-map	Eq. (19)	0.804	0.804	0.003	0.801–0.806	0.002	1.15

Notes. From left to right: mean value of Σ₈, value of Σ₈ at the maximum likelihood, standard deviation of Σ₈, 68% interval, systematic uncertainties, and χ² per degree of freedom.

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