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Table 2

Physical parameters of the observed clusters.

Cluster (U − B)ex NMS NPMS MF MFPMS AgePMS Σ Δ ΔLow   M ΔHigh   M
name Myr Myr pc pc pc
NGC 2362  −0.221 28 89  −0.74  ±  0.21  −2.30  ±  0.31 5.44 1.95 1.82 1.78 1.86
NGC 2367  −0.136 11 132  −1.13  ±  0.29  −1.95  ±  1.12 5.48 2.57 4.26 4.37 4.07
NGC 3293  −0.127 88 231  −0.64  ±  0.19  −1.63  ±  0.42 6.36 2.45 3.53 3.77 3.32
Collinder 228 0.105 16 305  −1.93  ±  0.25  −3.21  ±  0.27 6.46 2.53 3.60 3.52 3.68
Hogg 10  −0.050 20 270  −1.33  ±  0.47  −3.35  ±  0.51 6.31 2.47 3.25 3.26 3.08
Hogg 11 0.044 13 393  −1.20  ±  0.43  −3.88  ±  0.72 6.41 2.42 3.96 3.93 3.90
Trumpler 18  −0.097 16 126  −1.07  ±  0.29  −2.09  ±  0.58 4.59 2.84 2.01 2.04 2.18
NGC 3590  −0.123 37 406  −1.51  ±  0.34  −2.29  ±  0.35 6.28 2.43 2.98 2.98 2.94
NGC 4103 0.128 49 214  −1.31  ±  0.27  −2.41  ±  0.56 6.18 2.33 2.92 2.97 2.78
NGC 4463  −0.062 21 151  −1.35  ±  0.25  −3.75  ±  0.68 6.23 2.64 2.43 2.49 2.23
NGC 5606  −0.110 21 215  −1.53  ±  0.31  −3.40  ±  0.63 6.03 2.77 3.27 3.21 3.32

Notes. Column 1: cluster name; 2: (U − B) excess (Sect. 2.1); 3: number of MS+postMS members; 4: number of PMS members (Sect. 2.2); 5: slope of the mass functions, δlog NM/δlog M, for all the members of mass above the approximate completeness limit (Sect. 3.1.2); 6: the same slope for the mass function calculated with only the PMS members; 7, 8: average age of the PMS members (7), and its rms deviation (8); 9: average value of the distances between all pairs of PMS members; 10, 11: this same quantity calculated for the distribution of PMS members of low mass (1–2 M⊙) (10) and high mass (2–3.5 M⊙) (11).

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