Table A.1.
Summary of the average positional and kinematic properties of the clusters that were initially selected to be part of the CrA chain.
| CrA Main | CrA North | Sco Sting | Sco Body | V1062 Sco | η Lupus | ϕ Lupus | ||
|---|---|---|---|---|---|---|---|---|
| number of stars | total | 96 | 351 | 132 | 373 | 1029 | 769 | 1114 |
| RVs | 56 (23) (33) | 134 (126) (8) | 42 (40) (2) | 143 (139) (4) | 309 (309) (0) | 360 (357) (3) | 455 (455) (0) | |
| eRV< 3 | 24 (0) (24) | 32 (26) (6) | 7 (6) (1) | 25 (25) (0) | 58 (58) (0) | 69 (68) (1) | 86 (86) (0) | |
| eRV< 1 | 22 (0) (22) | 10 (6) (4) | 5 (4) (1) | 10 (10) (0) | 17 (17) (0) | 30 (29) (1) | 38 (38) (0) | |
| hel Cart. coord. [pc] | X | 148 | 145 | 132 | 139 | 167 | 124 | 112 |
| σX | 3 | 5 | 11 | 10 | 7 | 9 | 13 | |
| Y | -1 | -3 | -21 | -26 | -54 | -45 | -54 | |
| σY | 2 | 4 | 8 | 7 | 9 | 13 | 9 | |
| Z | -47 | -35 | -7 | 19 | 15 | 25 | 40 | |
| σZ | 2 | 7 | 9 | 12 | 5 | 9 | 9 | |
| [pc] | d* | 155 | 149 | 134 | 141 | 177 | 136 | 131 |
| hel Cart. vel. [km/s] | U | -4.5 | -5.5 | -5.9 | -3.1 | -3.9 | -4.6 | -5.0 |
| σU | 1.2 | 1.4 | 2.3 | 1.6 | 1.5 | 1.5 | 3.8 | |
| eUavg | 0.3 | 0.6 | 0.5 | 0.7 | 0.7 | 0.5 | 0.5 | |
| V | -17.8 | -17.4 | -19.0 | -16.8 | -19.6 | -19.9 | -19.8 | |
| σV | 0.8 | 0.6 | 0.5 | 0.6 | 0.4 | 1.2 | 1.7 | |
| eVavg | 0.3 | 0.1 | 0.1 | 0.1 | 0.2 | 0.2 | 0.3 | |
| W | -9.7 | -7.8 | -5.5 | -6.9 | -4.2 | -5.2 | -4.9 | |
| σW | 0.7 | 1.0 | 0.2 | 0.7 | 0.3 | 0.6 | 2.1 | |
| eWavg | 0.2 | 0.2 | 0.0 | 0.1 | 0.1 | 0.1 | 0.2 | |
| [Myr] | age** | 8.5 | 11.9 | 14.5 | 14.7 | 15.0 | 15.3 | 16.9 |
Notes. Rows 1–3 give the number of stars per cluster in total that have radial velocities, and how many stars remain after rejecting binary candidates and applying our error cuts of < 3 km s−1 and < 1 km s−1, respectively. In parentheses, we list the number of stars with radial velocities first from Gaia and second from APOGEE-2. The following statistics of the data are based on the heliocentric Cartesian coordinate system. Rows 4–9 list the mean positions and standard deviation per cluster, excluding binary candidates, low-stability stars, and sigma outliers, but including stars without radial velocity measurements. The cluster distance is taken directly from R23a. The mean standard deviation and average uncertainty of the velocities (rows 12–20) are taken from our sample of stars with radial velocity errors < 1 km s−1. Ages are listed as derived by R23b.
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