Table D.1.
Overview of the contamination fraction from older stars as estimated with different photometric quality criteria.
| Used Cuts | All | Young | Old |
|---|---|---|---|
| No Stability cut | |||
| In G, GBP, GRP (no cuts) | 12,724 | 11,122 (87.4%) | 1,602 (12.6%) |
| Eq. D.3 (looser cut) | 11,906 | 10,700 (89.9%) | 1,206 (10.1%) |
| Eq. D.2 (used in Fig. 14) | 11,162 | 10,402 (93.2%) | 760 (6.8%) |
| Eq. D.4 (stricter cut) | 9,636 | 9,227 (95.8%) | 409 (4.2%) |
| Stability > 11% | |||
| In G, GBP, GRP (no cuts) | 11,213 | 10,211 (91.1%) | 1,002 (8.9%) |
| Eq. D.3 (looser cut) | 10,621 | 9.873 (93.0%) | 748 (7.0%) |
| Eq. D.2 (used in Fig. 14) | 10,014 | 9,607 (95.9%) | 407 (4.1%) |
| Eq. D.4 (stricter cut) | 8,692 | 8,528 (98.1%) | 164 (1.9%) |
Notes. In parentheses we give the fraction of young and old stellar candidates relative to the number of sources after the individual photometric error cuts, given in column “All.” The top four rows show the estimates using sources with no stability cut, and the bottom four rows show the estimates using a cut at stability > 11%. We stress that this is not a generally suggested cut to get cleaner samples, since the maximum stability varies per cluster.
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