Table 2
Overview of reference values used in constructing the composite HRD for open clusters (Fig. 2).
| Cluster | DM | log(age) | [Fe/H] | E(B − V) | Memb |
|---|---|---|---|---|---|
| Hyades | 3.389 | 8.90 | 0.13 | 0.001 | 480 |
| Coma Ber | 4.669 | 8.81 | 0.00 | 0.000 | 127 |
| Pleiades | 5.667 | 8.04 | −0.01 | 0.045 | 1059 |
| IC 2391 | 5.908 | 7.70 | −0.01 | 0.030 | 254 |
| IC 2602 | 5.914 | 7.60 | −0.02 | 0.031 | 391 |
| α Per | 6.214 | 7.85 | 0.14 | 0.090 | 598 |
| Praesepe | 6.350 | 8.85 | 0.16 | 0.027 | 771 |
| NGC 2451A | 6.433 | 7.78 | −0.08 | 0.000 | 311 |
| Blanco 1 | 6.876 | 8.06 | 0.03 | 0.010 | 361 |
| NGC 6475 | 7.234 | 8.54 | 0.02 | 0.049 | 874 |
| NGC 7092 | 7.390 | 8.54 | 0.00 | 0.010 | 248 |
| NGC 6774 | 7.455 | 9.30 | 0.16 | 0.080 | 165 |
| NGC 2232 | 7.575 | 7.70 | 0.11 | 0.031 | 241 |
| NGC 2547 | 7.980 | 7.60 | −0.14 | 0.040 | 404 |
| NGC 2516 | 8.091 | 8.48 | 0.05 | 0.071 | 1727 |
| Trumpler 10 | 8.223 | 7.78 | −0.12 | 0.056 | 407 |
| NGC 752 | 8.264 | 9.15 | −0.03 | 0.040 | 259 |
| NGC 6405 | 8.320 | 7.90 | 0.07 | 0.139 | 544 |
| IC 4756 | 8.401 | 8.98 | 0.02 | 0.128 | 515 |
| NGC 3532 | 8.430 | 8.60 | 0.00 | 0.022 | 1802 |
| NGC 2422 | 8.436 | 8.11 | 0.09 | 0.090 | 572 |
| NGC 1039 | 8.552 | 8.40 | 0.02 | 0.077 | 497 |
| NGC 6281 | 8.638 | 8.48 | 0.06 | 0.130 | 534 |
| NGC 6793 | 8.894 | 8.78 | 0.272 | 271 | |
| NGC 2548 | 9.451 | 8.74 | 0.08 | 0.020 | 374 |
| NGC 6025 | 9.513 | 8.18 | 0.170 | 431 | |
| NGC 2682 | 9.726 | 9.54 | 0.03 | 0.037 | 1194 |
| IC 4651 | 9.889 | 9.30 | 0.12 | 0.040 | 932 |
| NGC 2323 | 10.010 | 8.30 | 0.105 | 372 | |
| NGC 2447 | 10.088 | 8.74 | −0.05 | 0.034 | 681 |
| NGC 2360 | 10.229 | 8.98 | −0.03 | 0.090 | 848 |
| NGC 188 | 11.490 | 9.74 | 0.11 | 0.085 | 956 |
Notes. Distance moduli (DM) as derived from the Gaia astrometry; ages and reddening values as derived from Gaia photometry (see Sect. 6), with distances fixed on astrometric determinations; metallicities from Netopil et al. (2016); Memb: the number of members with Gaia photometric data after application of the photometric filters.
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