Table 3.
Concentrations of the ensemble cluster and its subsamples.
| Sample | cν | cν, Q | cν, SF | c⋆ | c200 |
|---|---|---|---|---|---|
| ensemble | 3.1 ± 0.5 | 5.1 ± 0.9 | 0.7 ± 0.4 | 4.1 ± 0.7 | 3.2 ± (0.23, 0.12, 0.05) |
| low-M200 | 2.0 ± 0.6 | 4.7 ± 1.7 | 0.3 ± 0.4 | 2.3 ± 0.7 | 3.5 ± (0.20, 0.18, 0.24) |
| high-M200 | 4.2 ± 0.8 | 6.0 ± 1.4 | 1.2 ± 0.7 | 6.1 ± 1.3 | 3.1 ± (0.27, 0.15, 0.09) |
| low-z | 3.2 ± 0.7 | 5.8 ± 1.5 | 0.3 ± 0.4 | 2.0 ± 0.5 | 3.7 ± (0.43, 0.22, 0.21) |
| high-z | 3.2 ± 0.8 | 5.4 ± 1.7 | 1.5 ± 1.0 | 4.6 ± 1.2 | 2.7 ± (0.22, 0.17, 0.10) |
Notes. cν, cν, Q, and cν, SF are the concentrations of the best-fit NFW models to the number density profiles of all, quiescent, and star-forming galaxies, respectively. c⋆ is the concentration of the best-fit NFW model to the M⋆ density profile. c200 is the ℒ-weighted average of the concentrations of the 35 best-fit model M(r) obtained via the MAMPOSSt analysis. The three components to the total uncertainty on c200 are given in parentheses: δc, s, δc, ν, and δc, j, respectively (see Sect. 3.2 for their definitions).
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