Table 5
Dynamical mass estimates after the substructure analysis.
| Cluster | M 200 | R 200 |
|
MV(R200) |
|
Mc(R200) |
|
| (1015 M⊙) | (Mpc) | (1015 M⊙) | (1015 M⊙) | (1015 M⊙) | (1015 M⊙) | (1015 M⊙) | |
|
|
|||||||
| RXC J0014 |
|
|
|
|
|
|
|
| RXC J0225 |
|
|
|
|
|
|
|
| RXC J0516 |
|
|
|
|
|
|
|
| RXC J0528 |
|
|
|
|
|
|
|
| RXC J0658 |
|
|
|
|
|
|
|
| RXC J1131 |
|
|
|
|
|
|
|
| RXC J1206 |
|
|
|
|
|
|
|
| RXC J1347 |
|
|
|
|
|
|
|
| RXC J2011 |
|
|
|
|
|
|
|
| RXC J2308 |
|
|
|
|
|
|
|
Notes. Columns: (1) cluster name. (2) Best-fit NFW mass derived from the Jeans analysis. As for the first analysis, the best-fit model combines the NFW mass profile with one of the three different anisotropy models. (3) Corresponding NFW radius. (4) Extrapolation of the Jeans best-fit NFW profile to the radius 
obtained before the substructure analysis (i.e. fourth column of Table 2). (5, 6) Mass derived from the virial theorem within an aperture of radius R200 and . (7, 8) Caustic mass at the same two radii. The galaxy density in PPS, the density level κ, the velocity dispersion σP( <R), and the caustic amplitude were re-estimated accordingly. The masses given in Cols. 4, 6, and 8 are the values used in Sect. 5.5 to investigate the impact of substructures.
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