Table 2
Basic parameters obtained for the investigated clusters with the new filter process and cross-entropy (CE) method.
| Paper I | This work UBV | This work 2MASS | |||||||||
| Cluster | E(B − V) | Distance | Log(Age) | E(B − V) | Distance | Log(Age) | E(J − H) | E(B − V) | Distance | Log(Age) | |
| (mag) | (pc) | (yr) | (mag) | (pc) | (yr) | (mag) | (mag) | (pc) | (yr) | ||
|
|
|||||||||||
| NGC 2477 | 0.29 ± 0.03 | 1385 ± 64 | 8.90 ± 0.09 | 0.29 ± 0.02 | 1565 ± 103 | 8.83 ± 0.05 | 0.09 ± 0.03 | 0.27 ± 0.09 | 1300 ± 117 | 8.95 ± 0.08 | |
| NGC 7044 | 0.55 ± 0.02 | 3093 ± 345 | 9.35 ± 0.17 | 0.53 ± 0.01 | 3323 ± 116 | 9.32 ± 0.16 | 0.27 ± 0.03 | 0.82 ± 0.09 | 3115 ± 79 | 9.00 ± 0.12 | |
| NGC 2266 | 0.17 ± 0.02 | 3100 ± 244 | 8.90 ± 0.07 | 0.15 ± 0.01 | 3285 ± 289 | 8.82 ± 0.08 | 0.07 ± 0.03 | 0.21 ± 0.09 | 2855 ± 155 | 9.00 ± 0.12 | |
| Berkeley 32 | 0.12 ± 0.04 | 3483 ± 186 | 9.65 ± 0.13 | 0.14 ± 0.02 | 3271 ± 83 | 9.62 ± 0.13 | 0.06 ± 0.02 | 0.18 ± 0.06 | 3122 ± 170 | 9.55 ± 0.14 | |
| NGC 2682 | 0.02 ± 0.01 | 774 ± 225 | 9.55 ± 0.05 | 0.03 ± 0.01 | 765 ± 52 | 9.48 ± 0.23 | 0.08 ± 0.04 | 0.24 ± 0.12 | 722 ± 82 | 9.05 ± 0.17 | |
| 0.05 ± 0.01 | 758 ± 226 | 9.60 ± 0.06 | 0.10 ± 0.02 | 802 ± 30 | 9.05 ± 0.28 | ||||||
| 0.04 ± 0.01 | 869 ± 557 | 9.50 ± 0.07 | 0.04 ± 0.01 | 792 ± 20 | 9.45 ± 0.08 | ||||||
| NGC 2506 | 0.03 ± 0.01 | 3587 ± 198 | 9.20 ± 0.05 | 0.03 ± 0.04 | 3349 ± 795 | 9.20 ± 0.16 | 0.06 ± 0.01 | 0.18 ± 0.03 | 2966 ± 127 | 9.15 ± 0.09 | |
| 0.07 ± 0.01 | 3137 ± 177 | 9.25 ± 0.05 | 0.05 ± 0.01 | 3533 ± 144 | 9.10 ± 0.10 | ||||||
| NGC 2355 | 0.25 ± 0.02 | 2316 ± 103 | 8.80 ± 0.05 | 0.26 ± 0.01 | 2083 ± 243 | 8.82 ± 0.10 | 0.10 ± 0.03 | 0.30 ± 0.09 | 1985 ± 144 | 8.90 ± 0.08 | |
| 0.19 ± 0.02 | 2022 ± 88 | 8.85 ± 0.05 | 0.18 ± 0.02 | 2213 ± 238 | 8.85 ± 0.07 | ||||||
| Melotte 105 | 0.47 ± 0.02 | 1750 ± 111 | 8.40 ± 0.06 | 0.48 ± 0.02 | 1701 ± 329 | 8.48 ± 0.18 | 0.11 ± 0.01 | 0.33 ± 0.03 | 1739 ± 244 | 8.75 ± 0.15 | |
| 0.49 ± 0.03 | 2005 ± 139 | 8.45 ± 0.07 | 0.57 ± 0.06 | 1910 ± 285 | 8.48 ± 0.18 | ||||||
| Trumpler 1 | 0.59 ± 0.05 | 2419 ± 185 | 7.85 ± 0.19 | 0.62 ± 0.04 | 2145 ± 78 | 7.75 ± 0.25 | 0.15 ± 0.06 | 0.45 ± 0.18 | 1880 ± 490 | 7.70 ± 0.30 | |
| 0.53 ± 0.03 | 2309 ± 121 | 7.55 ± 0.31 | 0.62 ± 0.04 | 2339 ± 146 | 7.00 ± 0.18 | ||||||
| Dias 6 | 0.87 ± 0.03 | 2239 ± 213 | 8.85 ± 0.09 | 0.29 ± 0.02 | 0.89 ± 0.06 | 2423 ± 324 | 8.80 ± 0.11 | ||||
Notes. In the first three columns (after the cluster identification) we reproduce the results published in Paper I to make comparison easy. Then the results are given using UBV data from the literature and using 2MASS data. E(B − V) is the extinction, d the distance to the cluster, log (Age) the logarithm of the age (in years). The sequence of the references is the same as presented in Table 1, and the WEBDA reference codes are given in Paper I. The adopted metallicity is solar (Z = 0.019) for NGC 2477, NGC 7044, NGC 2682, Melotte 105 and Trumpler 1, and Z = 0.008 for NGC 2266, Berkeley 32, NGC 2506, and NGC 2355. Table 1 gives the used radius to extracted 2MASS data and the CE fit parameters. The E(B − V) obtained from the 2MASS data were computed using E(J − H)/E(B − V) = 0.33, and the errors obtained by the traditional propagation error theory.
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