Table 1
Parameters of the young stellar associations considered for the detectability assessment.
| No. stars | ||||||
|---|---|---|---|---|---|---|
| Association | d (pc) | Age (Myr) | A | G | M | Ref. |
| AB Doradus | 20 | 150 | 0 | 23 | 8 | 3 |
| β Pictorisa | 37a | 23 | 6 | 16 | 9 | 1a |
| β Tucanae | 43 | 45 | 4 | 0 | 1 | 4 |
| Tucana Horologium | 48 | 45 | 2 | 27 | 5 | 2,5 |
| Columba | 50 | 42 | 2 | 37 | 1 | 2 |
| TW Hydrae | 53 | 10 | 2 | 0 | 33 | 6 |
| Carina | 65 | 45 | 0 | 22 | 0 | 2 |
| 32 Orionis | 92 | 22 | 2 | 7 | 2 | 7,8 |
| η Chamaeleontis | 94 | 11 | 1 | 0 | 11 | 2 |
| χ1 For | 99 | 50 | 2 | 0 | 0 | 9 |
Notes. Thedistances (d) and ages of the stellar associations are from Mamajek (2016) and references therein. (a) For the β Pictoris moving group we computed the mean distances from a combined list of Tables 1 and 2 of Mamajek & Bell (2014), and took the spectral types from the SIMBAD database where they were not provided. The mean distance of 15 pc given in Mamajek (2016) seems to be a typo.
References. A-, G-, and M-star members: (1) Mamajek & Bell (2014), (2) Torres et al. (2008), (3) Zuckerman et al. (2011), (4) Wenger et al. (2000), (5) Kraus et al. (2014), (6) Gagné et al. (2017), (7) Bell et al. (2017), (8) Shvonski et al. (2016), (9) Mamajek (2016). We consider only bona fide stellar members to be conservative.
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