Table D.1
Cluster parallaxes.
| Cluster | π | std.dev. | spat.corr. | depth | size | N | π | Remark |
|---|---|---|---|---|---|---|---|---|
| (µas) | (µas) | (µas) | (µas) | (′) | (mas) | |||
| Marigo et al. (This work) | ||||||||
| Berkeley 9 | 586.8 ± 12.5 | 58.99 | 10.95 | 0.90 | 5.3 | 101 | 0.52-0.65 (0.53-0.65) | |
| Berkeley 14 | 234.4 ± 12.6 | 66.45 | 10.95 | 0.35 | 5.1 | 118 | 0.15-0.30 (0.17-0.30) | |
| Berkeley 29 | 83.2 ± 19.0 | 71.23 | 10.95 | 0.25 | 10.2 | 21 | ||
| Berkeley 34 | 160.2 ± 16.0 | 78.68 | 10.95 | 0.11 | 2.4 | 45 | 0.12-0.27 (0.08-0.24) | |
| Berkeley 53 | 301.9 ± 12.0 | 84.14 | 10.94 | 2.11 | 24.0 | 358 | 0.22-0.37 (0.22-0.39) | * |
| Berkeley 54 | 159.4 ± 12.9 | 68.16 | 10.95 | 0.24 | 5.1 | 102 | * | |
| Berkeley 72 | 203.5 ± 13.8 | 89.50 | 10.94 | 0.81 | 13.6 | 113 | 0.11-0.25 (0.11-0.29) | |
| Berkeley 91 | 256.9 ± 17.4 | 81.21 | 10.95 | 0.26 | 3.5 | 36 | ||
| BH 55 | 250.1 ± 12.7 | 63.42 | 10.95 | 0.38 | 5.2 | 95 | 0.19-0.30 (0.19-0.31) | |
| BH 67 | 156.9 ± 13.9 | 61.06 | 10.95 | 0.12 | 2.5 | 51 | 0.07-0.20 (0.10-0.22) | * |
| BH 92 | 423.8 ± 12.1 | 34.81 | 10.95 | 0.28 | 2.3 | 47 | ||
| BH 99 | 2269.0 ± 23.6 | 45.52 | 10.91 | 20.80 | 31.5 | 301 | ||
| Collinder 74 | 403.2 ± 11.9 | 50.81 | 10.95 | 0.83 | 7.0 | 119 | * | |
| Czernik 37 | 411.5 ± 11.7 | 61.50 | 10.95 | 0.81 | 6.8 | 245 | ||
| Dias 2 | 248.9 ± 15.5 | 81.38 | 10.95 | 0.56 | 7.7 | 55 | 0.18-0.32 (0.17-0.33) | * |
| FSR 154 | 264.0 ± 11.9 | 48.90 | 10.95 | 0.43 | 5.6 | 114 | * | |
| FSR 172 | 332.5 ± 12.0 | 38.89 | 10.95 | 0.28 | 2.9 | 63 | 0.30-0.37 (0.29-0.37) | |
| FSR 1521 | 281.1 ± 13.0 | 64.92 | 10.95 | 0.34 | 4.2 | 88 | * | |
| FSR 1530 | 281.6 ± 19.7 | 94.39 | 10.95 | 0.29 | 3.6 | 33 | * | |
| Gulliver 16 | 233.0 ± 12.3 | 46.39 | 10.95 | 0.48 | 7.1 | 69 | ||
| Haffner 14 | 274.5 ± 11.6 | 37.80 | 10.95 | 1.36 | 17.0 | 114 | 0.25-0.31 (0.24-0.31) | * |
| IC 1311 | 158.0 ± 11.2 | 49.60 | 10.95 | 0.24 | 5.2 | 504 | ||
| Juchert Saloran 1 | 209.0 ± 13.2 | 62.27 | 10.95 | 0.45 | 7.4 | 73 | 0.16-0.29 (0.15-0.27) | |
| King 11 | 339.0 ± 11.6 | 59.12 | 10.95 | 0.43 | 4.4 | 262 | 0.27-0.40 (0.28-0.40) | * |
| Melotte 66 | 219.1 ± 11.3 | 55.53 | 10.95 | 0.49 | 7.7 | 404 | * | |
| NGC 559 | 358.1 ± 11.2 | 47.32 | 10.95 | 0.63 | 6.1 | 528 | * | |
| NGC 663 | 371.5 ± 11.2 | 33.70 | 10.94 | 1.98 | 18.3 | 750 | 0.35-0.40 (0.34-0.41) | |
| NGC 743 | 942.7 ± 11.7 | 26.27 | 10.95 | 2.18 | 7.9 | 60 | ||
| NGC 1798 | 240.2 ± 11.6 | 59.28 | 10.95 | 0.44 | 6.3 | 241 | 0.19-0.28 (0.18-0.30) | |
| NGC 2345 | 392.2 ± 11.2 | 41.70 | 10.95 | 1.25 | 11.0 | 513 | ||
| NGC 2506 | 315.6 ± 11.1 | 52.36 | 10.95 | 0.71 | 7.8 | 1447 | * | |
| NGC 2516 | 2455.7 ± 25.8 | 33.84 | 10.92 | 23.37 | 32.7 | 400 | ||
| NGC 2533 | 381.7 ± 11.3 | 29.90 | 10.95 | 0.79 | 7.1 | 119 | 0.36-0.41 (0.35-0.41) | |
| NGC 2660 | 367.2 ± 11.1 | 38.63 | 10.95 | 0.34 | 3.2 | 426 | 0.32-0.41 (0.33-0.41) | |
| NGC 5662 | 1327.6 ± 13.8 | 37.29 | 10.93 | 8.12 | 21.0 | 249 | ||
| NGC 6242 | 805.9 ± 11.4 | 50.65 | 10.95 | 2.24 | 9.5 | 481 | ||
| NGC 6649 | 507.4 ± 11.2 | 57.97 | 10.95 | 0.77 | 5.2 | 594 | ||
| NGC 7654 | 636.1 ± 11.2 | 31.67 | 10.95 | 1.96 | 10.6 | 1008 | ||
| NGC 7789 | 481.3 ± 30.4 | 63.32 | 10.95 | 1.53 | 10.9 | 5 | 0.47-0.54 (0.42-0.54) | |
| Pismis 3 | 473.2 ± 11.3 | 49.92 | 10.95 | 1.36 | 9.9 | 356 | 0.42-0.53 (0.42-0.52) | * |
| Ruprecht 37 | 216.6 ± 12.8 | 61.55 | 10.95 | 0.19 | 3.0 | 88 | 0.16-0.27 (0.16-0.28) | * |
| Ruprecht 42 | 189.4 ± 12.6 | 60.30 | 10.95 | 0.36 | 6.6 | 94 | ||
| Ruprecht 83 | 287.4 ± 11.6 | 41.81 | 10.95 | 0.35 | 4.2 | 126 | ||
| Ruprecht 91 | 973.4 ± 12.1 | 29.55 | 10.94 | 4.72 | 16.7 | 160 | ||
| Ruprecht 107 | 283.8 ± 11.6 | 32.14 | 10.95 | 0.34 | 4.1 | 71 | ||
| Ruprecht 112 | 382.8 ± 11.1 | 36.47 | 10.95 | 1.11 | 9.9 | 455 | * | |
| SAI 47 | 228.4 ± 17.4 | 59.16 | 10.95 | 0.19 | 2.8 | 19 | ||
| Teutsch 106 | 166.5 ± 12.1 | 46.06 | 10.95 | 0.20 | 4.1 | 83 | ||
| Tombaugh 1 | 426.4 ± 11.5 | 31.01 | 10.95 | 0.95 | 7.6 | 85 | 0.39-0.45 (0.40-0.46) | |
| Tombaugh 2 | 140.3 ± 11.7 | 66.82 | 10.95 | 0.14 | 3.4 | 266 | * | |
| Trumpler 5 | 336.5 ± 11.6 | 86.14 | 10.94 | 1.83 | 18.7 | 713 | 0.26-0.41 (0.25-0.42) | * |
Notes. Column 1: Cluster name. Column 2: Cluster parallax and adopted error. The error is calculated as the standard deviation in Col. 3 divided by the square root of the number of selected members in Col. 7, added in quadrature to the numbers in Cols. 4 and 5. Column 3: Standard deviation in the cluster parallax. Column 4: Floor in the cluster parallax error due to the spatial covariance. Column 5: Depth effect due to the size of the cluster. Column 6: Size of the cluster (defined as containing 68% of the selected members). Column 7: Total number of selected stars. Column 8: Cluster parallax according to Marigo et al. (2022) including the Lindegren et al. (2021) correction and quoted as the 68% confidence interval (from their table 10). Between parenthesis our result is quoted based on the median and the standard deviation in Column 3 and using the same format. Column 9: An asterisks indicates that the AGB star(s) in the cluster is (are) in the MW sample and that the parallax was updated with that of the cluster.
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