Table 6.
Possible clusters as sites of origin of the Halo runaway stars using spatial coincidence.
| Star | Cluster Name | p-val | Tf | Trel | vrel | Tc | Flagage | Suggested | References | |
|---|---|---|---|---|---|---|---|---|---|---|
| (Myr) | (Myr) | (km s−1) | (Myr) | mechanism | ||||||
| HIP 60350 | Cl Pismis 19 | 0.40 | −14.3 | – | 403 | 1000 ± 230 | N | – | 1,2,5 | |
| Cl Pismis 20 | 0.43 | −14.98 | 9.90 ± 0.13 | 376 | < 50 | Y | DES | 1,2,6 | ||
| NGC 5617 | 0.002 | −13.28 | – | 378 | 199.5 ± 68.8 | N | – | 1,2,5 | ||
| PG 1332+137 (a) | Sai 132 | 0.99 | −20.7 | – | 272 | 500 | N | – | 1,2,7 | |
| PHL 159 | Cl Basel 2 | 0.73 | −24.9 | – | 137.4 | 560 ± 70 | N | – | 1,2,8 | |
| PB 5418 | Cl Gulliver 43 | 0.67 | −23.6 | 25.72 ± 1.45 | 238 | – | – | BSS | 1,2 | |
| HIP 70275 | NGC 1502 | 0.52 | −11.2 | 11.44 ± 0.39 | 260 | 11.0 ± 0.7 | Y | DES | 1,3,9,10 | |
| HIP 11809 | [FSR2007] 0883 | 0.05 | −10.2 | – | 268.4 | 700 ± 42 | N | – | 1,4,10 | |
| HIP 114569 (b) | Cl VDBH 217 | – | −7 | 7.52 ± 1.21 | – | 40 ± 10 | Y | BSS | 1,2,11 | |
| HIP 105912 | Teutsch 145 | 0.66 | −13.9 | – | 202.3 | 500 | N | – | 1,2,7 | |
| BD-02 3766 | Kronberger 38 | 0.54 | −14.7 | 16.18 ± 1.08 | 338.1 | – | – | DES | 1,2 | |
| BD-15 115 | Juchert 3 | 0.52 | −32 | 30.54 ± 0.87 | 202.2 | – | – | DES | 1,2 | |
| NGC 6755 | 0.016 | −30.8 | – | 194.3 | 174.0 ± 10.4 (c) | N | – | 1,2,11,12 |
Notes. The columns show the p-values for EDR3 proper motions along with the expected time of flight Tf in Myr, and the relative velocities vrel in km s−1. Tc is the age of the clusters in Myr. We use the column Flagage for a temporal origin based on the cluster age, with ‘Y’ meaning the cluster may be a possible site of origin, and ‘N’ meaning it cannot be a site since it is too old.
The star has a RUWE of 1.48 in EDR3. We therefore also ran the fit with DR2 data which has a RUWE of 0.99. The results did not change for the latter.
References. Kinematic of clusters/associations: (1) Cantat-Gaudin & Anders (2020); (2) RV Soubiran et al. (2018); (3) Conrad et al. (2017); (4) Carrera et al. (2019); Age estimates of Clusters: (5) Angelo et al. (2021); (6) Dib et al. (2018); (7) Netopil & Paunzen 2013; (8) Glushkova et al. (2010); (9) Yu et al. (2018); (10) Liu & Pang (2019); (11) Clariá et al. (2019); (12) Alonso-Santiago et al. (2020).
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