Table 1.
Derived parameters for the star clusters.
| Cluster | Age | [Fe/H]CMD | [Fe/H]CaT | E(B − V) | Dist. | a | αJ2000 | δJ2000 | RVhel | μα ⋅ cos(δ) | μδ |
|---|---|---|---|---|---|---|---|---|---|---|---|
| ±unc.(std.dev.) | ±unc.(std.dev.) | ±unc.(std.dev.) | ±unc.(std.dev.) | ||||||||
| name | (Gyr) | (dex) | (dex) | (mag) | (kpc) | (deg) | hh:mm:ss | dd:mm:ss | (km s−1) | (mas yr−1) | (mas yr−1) |
| Magellanic Bridge | |||||||||||
| BS 196 |
 |
 |
−0.89 ± 0.04(0.08) |
 |
 |
5.978 | 01:48:01.8 | −70:00:13 | 135.5 ± 1.4(2.7) | 1.12 ± 0.07(0.18) | −1.14 ± 0.06(0.05) |
| BS 188( * ) |
 |
 |
−0.94 ± 0.06(0.13) |
 |
 |
4.441 | 01:35:10.9 | −71:44:11 | 120.3 ± 3.5(7.9) | 1.25 ± 0.08(0.23) | −1.35 ± 0.07(0.04) |
| HW 56( * *) |
 |
 |
−0.97 ± 0.12(0.20) |
 |
 |
2.397 | 01:07:41.1 | −70:56:06 | 157.7 ± 5.4(9.3) | 0.99 ± 0.11(0.04) | −1.27 ± 0.10(0.29) |
| HW 85 |
 |
 |
−0.82 ± 0.06(0.14) |
 |
 |
5.219 | 01:42:28.0 | −71:16:44 | 143.2 ± 3.0(6.8) | 1.26 ± 0.09(0.47) | −1.41 ± 0.09(0.26) |
| Lindsay 100 |
 |
 |
−0.89 ± 0.06(0.14) |
 |
 |
2.556 | 01:18:16.9 | −72:00:06 | 145.8 ± 1.4(3.3) | 0.98 ± 0.05(0.15) | −1.10 ± 0.05(0.11) |
| Transition | |||||||||||
| Bruck 168 |
 |
 |
−1.08 ± 0.06(0.09) |
 |
 |
3.584 | 01:26:42.7 | −70:47:01 | 141.7 ± 4.6(7.9) | 0.94 ± 0.09(0.08) | −1.15 ± 0.09(0.04) |
| Counter-Bridge | |||||||||||
| IC 1708 |
 |
 |
−1.11 ± 0.06(0.17) |
 |
 |
3.286 | 01:24:55.9 | −71:11:04 | 214.9 ± 2.7(6.6) | 0.39 ± 0.10(0.35) | −1.26 ± 0.07(0.20) |
Notes. Age, [Fe/H]CMD, E(B − V), distance from VISCACHA CMD isochrone fitting, [Fe/H]CaT, RVhel from GMOS spectra, μα, and μδ from Gaia EDR3. Distance a follows the definition by Dias et al. (2014), and (α, δ) coordinates are from Bica et al. (2020). ( * )BS 188 was observed under sub-optimal weather conditions, and the resulting isochrone fitting is very sensitive to a handful of stars from the shallow CMD, which could explain the metallicity difference between photometric and spectroscopic [Fe/H] (see Appendix A.1). ( * *)HW 56 is immersed in a dense field (a = 2.397°, the smallest in our sample) that has a very similar CMD as the cluster region; therefore, the statistical decontamination left low-probable member stars on the fainter main sequence region, which may bias the photometric metallicities (see Appendix A.1). These uncertainties do not change the conclusions of this work.
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