CODEX: Role of velocity substructure in the scaling relations of galaxy clusters

Open Access

Table 4.

Summary of regression analysis for velocity dispersion (obtained using the gapper method) vs. the X-ray luminosity scaling relation for the SCGF sample.

Sample	Intercept α	Slope β	Intrinsic scatter σ	N clusters
Full sample	6.555 ± 0.018	0.168 ± 0.016	0.163 ± 0.016	530
z ≥ 0.3	6.599 ± 0.154	0.172 ± 0.137	0.073 ± 0.060	45
0.15 ≤ z < 0.3	6.552 ± 0.033	0.195 ± 0.048	0.073 ± 0.042	156
z < 0.15	6.526 ± 0.028	0.148 ± 0.024	0.191 ± 0.021	329
Gaussian z ≥ 0.3	6.564 ± 0.164	0.199 ± 0.144	0.081 ± 0.063	39
Gaussian 0.15 ≤ z < 0.3	6.549 ± 0.037	0.187 ± 0.052	0.070 ± 0.043	130
Gaussian z < 0.15	6.494 ± 0.028	0.137 ± 0.023	0.156 ± 0.023	263
Gaussian z ≥ 0.3, λ ≥ 47.2	6.590 ± 0.149	0.181 ± 0.128	0.076 ± 0.065	39
Gaussian 0.15 ≤ z < 0.3, λ ≥ 47.2	6.563 ± 0.034	0.187 ± 0.048	0.062 ± 0.046	116
Gaussian z < 0.15, λ ≥ 47.2	6.589 ± 0.038	0.091 ± 0.041	0.213 ± 0.035	90
Gaussian z ≥ 0.3, L_X ≥ 10⁴⁴ [ergs s⁻¹]	6.556 ± 0.168	0.204 ± 0.136	0.080 ± 0.071	39
Gaussian 0.15 ≤ z < 0.3, L_X ≥ 10⁴⁴ [ergs s⁻¹]	6.557 ± 0.056	0.174 ± 0.066	0.073 ± 0.057	97
Gaussian z < 0.15, L_X ≥ 10⁴⁴ [ergs s⁻¹]	6.505 ± 0.077	0.099 ± 0.077	0.168 ± 0.047	54

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