Table 8
Mass estimates of the clusters.
| Exemplar | Double Irony | Note | |
|---|---|---|---|
| N(R <6.′3) | 46 | 55 | (1) |
| N (<6.′3, 0.13 < z < 0.15) | 23 | 32 | (2) |
| zcluster | 0.1387 | 0.1368 | (3) |
| σv[km s−1] | 475 | 275 | (4) |
| MCaustic[M⊙] | 3.2 × 1014 | 9.1 × 1013 | (5) |
| M200[M⊙] | 1.7 × 1014 | 3.3 × 1013 | (6) |
| M500[M⊙] | 1.3 × 1014 | 2.5 × 1013 | (7) |
 |
(0.9 ± 0.4) × 1014 | <5.1 × 1013 | (8) |
Notes. (1) Total number of galaxies within a radius 6.3′ of the cluster center. (2) Number of galaxies within a radius 6.3′ of the cluster center and with 0.13 < z < 0.15. (3) Redshift estimate of the cluster. (4) Velocity dispersion estimated via the gapper method (Eq. 8). (5) Mass derived via the caustic method. (6) Mass within r200 derived via the mass–σ200 scaling relation (Eq. 9). (7) Mass within r500 scaled from M200 estimated via the scaling relation (Eq. 11). (8) Mass within r500 derived from X-rays (Table 2 for the Exemplar, and upper limit for the Double Irony, Table 5). The caustic mass estimates are higher than those derived via a simple scaling relation between the mass and the velocity dispersion, and also higher than those derived from X-rays. This apparent discrepancy is not surprising given the relatively small number of galaxies within the structures.
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