Table 5
Velocity dispersion estimates obtained with the maximum likelihood procedure described in the text using the Nelder–Meadmethod, except those indicated by an asterisk (where the Newton Conjugate Gradient method was employed).
| IC 2602 | IC 2391 | IC 4665 | NGC 2547 | |
|---|---|---|---|---|
| Ni | 66 | 43 | 16 | 34 |
| σv [km s-1] | 0.48 ± 0.04 | 0.59 ± 0.06 | 0.18 ± 0.04 | 0.43 ± 0.08 |
| Nf | 63 | 42 | 15 | 34 |
| σv [km s-1] | 0.20 ± 0.02 | 0.43 ± 0.05 | 0.03 ± 0.04 | 0.43 ± 0.08 |
| σ⊥[km s-1] | 0.32 ±0.02 | 0.42 ± 0.05 | 0.10 ± 0.02 | 0.60 ± 0.10 |
 |
38 | 22 | 10 | 17 |
| σv [km s-1] | 0.18 ± 0.02 | 0.20 ± 0.04 | 0.05 ± 0.03 | 0.24 ± 0.08 (*) |
 |
37 | 22 | 10 | 17 |
| σv [km s-1] | 0.16 ± 0.02 | 0.20 ± 0.04 | 0.05 ± 0.03 | 0.24 ± 0.08 (*) |
| σ⊥[km s-1] | 0.24 ± 0.02 | 0.30 ± 0.05 | 0.13 ± 0.03 | 0.40 ± 0.10 |
Notes. The quoted errors are obtained using the Cramér–Rao inequality. The first row lists the initial number of stars, from G17. The second row gives the values of σv estimated using the stars from the first row. The third row gives the number of stars remaining after the exclusion procedure, and the fourth and fifth rows give σv and σ⊥. The second half of the table is the same as the first half, except for the initial number of stars. Row six lists the number of stars within the radii from the cluster center given in Table 7.
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