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Table 6.
Best high Galactic latitude (|b| > 30°) hypervelocity star candidates (I).
| Gaia DR2 designation | α | δ | l | b | π | μα | μδ | Vr |
|---|---|---|---|---|---|---|---|---|
| (°) | (°) | (°) | (°) | (mas) | (mas yr−1) | (mas yr−1) | (km s−1) | |
| 1314483506970781824 | 251.80005602927 | +34.09044416258 | 56.12871617510 | +39.48243476824 | 0.0211 ± 0.0192 | −2.876 ± 0.028 | −4.863 ± 0.037 | −250.07 ± 0.73 |
| 1331376987735140864 | 248.87279142999 | +37.21051070025 | 59.84507313050 | +42.21970456491 | 0.0225 ± 0.0153 | −2.472 ± 0.022 | −5.669 ± 0.026 | −116.30 ± 2.12 |
| 1353387698695201792 | 256.23459332334 | +39.47807346868 | 63.53398480591 | +36.70985332927 | 0.0202 ± 0.0125 | −3.721 ± 0.021 | +0.654 ± 0.023 | −115.04 ± 0.89 |
| 1360405705322797312 | 259.28463512742 | +43.15993767132 | 68.36783292048 | +34.85872854418 | 0.0275 ± 0.0211 | −4.538 ± 0.037 | −0.371 ± 0.040 | −116.75 ± 1.02 |
| 1409724578557941248 | 245.96492962581 | +45.85548579341 | 71.74122097135 | +44.37334749643 | 0.0154 ± 0.0137 | −1.060 ± 0.023 | −4.180 ± 0.031 | −220.07 ± 1.98 |
| 1417386319177949824 | 268.14211061898 | +54.63524890374 | 82.57367537620 | +30.17952098747 | 0.0290 ± 0.0218 | −3.379 ± 0.048 | −5.631 ± 0.042 | −284.40 ± 1.59 |
| 1438071495854426880 | 253.13412753466 | +60.12250785829 | 89.65213628261 | +37.96715431762 | 0.0272 ± 0.0246 | −6.268 ± 0.038 | −0.483 ± 0.050 | −96.89 ± 0.72 |
| 1635042136319192576 | 251.91264273176 | +64.99736996879 | 95.80257919212 | +37.35065366127 | 0.0213 ± 0.0146 | −2.434 ± 0.024 | −1.501 ± 0.030 | −312.25 ± 1.30 |
| 1696697285206197248 | 236.71959038696 | +73.23047076409 | 108.14355244960 | +38.44334319408 | 0.0248 ± 0.0134 | −4.688 ± 0.026 | +1.991 ± 0.024 | +11.81 ± 1.69 |
| 3791385339777413504 | 167.47408084540 | −01.78401513372 | 258.65578792586 | +52.13596520194 | 0.0294 ± 0.0230 | −0.712 ± 0.047 | −5.779 ± 0.030 | −90.79 ± 1.69 |
Notes. The candidates here belong to the sample of 174 sources, which are probably distant and have the best astrometric solutions. Data source as in Table 2.
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