Table 2
Mean velocities and velocity dispersions.
| Sample | N |
|
σ v | TI |
| km s-1 | km s-1 | |||
|
|
||||
| Total | 222 | 0 ± 40 |
|
1.07 |
| DSb group | 10 | 584 ± 95 |
|
– |
| No-DSb | 205 | − 60 ± 40 |
|
1.05 |
| Inner | 88 | − 205 ± 66 |
|
0.88 |
| KMM-main | 63 | 73 ± 56 |
|
0.93 |
| KMM-sub | 25 | − 924 ± 39 |
|
0.94 |
| Outer | 117 | 28 ± 46 |
|
1.02 |
Notes. Values of the rest-frame mean velocity, the line-of-sight velocity dispersion, and the Tail Index (TI; see text) of the cluster as a whole and split in several subsamples, and of the detected substructures. The mean velocity and the velocity dispersion are computed using the robust biweight estimator (Beers et al. 1990). N is the number of objects in each sample. There are 17 DSb galaxies, of which 10 form a group, indicated as “DSb group” in the Table. The “No-DSb” sample is obtained from the “Total” after removal of the 17 DSb galaxies. “Inner” and “Outer” are subsamples of “No-DSb”, separated in radial distance by the value of 
. “KMM-main” and “KMM-sub” are subsamples of “Inner”, identified with the KMM algorithm, and separated in velocity space by the value − 621 km s-1.
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