Table 1
Cluster sample.
| SpARCS | N z | N m |
|
σ los | r 200 |
| number | [km s-1] | [kpc] | |||
|
|
|||||
| 0034 | 137 | 40 | 0.866 |
|
888 ± 110 |
| 0035 | 49 | 21 | 1.336 |
|
977 ± 154 |
| 0036 | 119 | 48 | 0.869 |
|
1230 ± 129 |
| 0215 | 125 | 46 | 1.004 |
|
953 ± 103 |
| 1047 | 147 | 29 | 0.956 |
|
926 ± 138 |
| 1051 | 145 | 32 | 1.034 |
|
705 ± 102 |
| 1613 | 161 | 83 | 0.872 |
|
1663 ± 130 |
| 1616 | 162 | 43 | 1.155 |
|
854 ± 107 |
| 1634 | 125 | 48 | 1.177 |
|
1008 ± 131 |
| 1638 | 112 | 38 | 1.195 |
|
769 ± 117 |
Notes. Nz is the number of galaxies with z in each cluster field (see Table 1 in Muzzin et al. 2012), Nm the number of cluster members. The mean redshift and line-of-sight velocity dispersion σlos, are computed on all cluster members. The 1σ error on is < 0.001 for all clusters. The virial radius r200 is computed from σlos using the iterative procedure of Mamon et al. (2013).
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