Table 1
Properties of the modelled clusters.
| ID | Profile | M s | No. stars |
|
N sim | Error (%) |
|
|
||||||
| P0 | Plummer | single | 30 000 | 1.3 | 15 | 0.5 |
| P1 | Plummer | IMF | 30 000 | 1.3 | 15 | 2–3 |
| LK0 | King | single | 30 000 | 1.3 | 15 | 2–3 |
| LK1 | King | IMF | 30 000 | 1.3 | 15 | 2–3 |
| LK2 | King | IMF | 30 000 | 4.6 | 15 | 2–3 |
| LK3 | King | IMF | 45 000 | 1.3 | 15 | 2–3 |
| LK4 | King | IMF | 15 000 | 1.3 | 15 | 2–3 |
| CK1 | King | IMF | 30 000 | 0.1 | 7 | 3–4 |
| CK2 | King | IMF | 30 000 | 0.2 | 5 | 3–4 |
| CK3 | King | IMF | 30 000 | 0.3 | 5 | 3–4 |
| CK4 | King | IMF | 30 000 | 0.5 | 5 | 3–4 |
Notes.The first column ID, stands for the identifier; the second column shows the shape of the used cluster profile; the third column Ms is the distribution of stellar masses where IMF implies the Kroupa 2001 version; the forth column is the number of stars; the fifth column shows the initial half-mass radius in pc; the sixth and seventh columns show the number of simulations performed for the given set-up and the resulting standard deviation.
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