Table 3
Virial masses and radii before the substructure analysis.
| Cluster | pop. | zspec | σtot | σ P | M V | R V | M 200 | R 200 | M σ |
| (km s-1) | (km s-1) | (1015M⊙) | (Mpc) | (1015M⊙) | (Mpc) | (1015M⊙) | |||
|
|
|||||||||
| RXC J0225 | all | 0.2189 ± 0.0003 |
|
|
|
|
|
|
|
| red | 0.2195 ± 0.0003 |
|
|
|
|
|
|
|
|
|
|
|||||||||
| RXC J0528 | all | 0.2837 ± 0.0003 |
|
|
|
|
|
|
|
| red | 0.2832 ± 0.0004 |
|
|
|
|
|
|
|
|
|
|
|||||||||
| RXC J2308 | all | 0.2968 ± 0.0003 |
|
|
|
|
|
|
|
| red | 0.2967 ± 0.0004 |
|
|
|
|
|
|
|
|
Notes. Columns: (1) cluster name. (2) Galaxy population. (3) Spectroscopic redshift. (4) Line-of-sight velocity dispersion within the entire FOV. (5) Line-of-sight velocity dispersion within the virial radius. (6) Cluster mass estimated from the virial theorem. (7) Virial radius estimated from Eq. (4). (8) Cluster mass estimated from the virial theorem, within an overdensity Δ = 200. (9) Cluster radius, estimated from Eq. (4)for Δ = 200. (10) Cluster mass estimated from the scaling relation of Biviano et al. (2006), i.e. Mσ = M(σP,200) with σP,200 the line-of-sight velocity dispersion estimated within R200.
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