Table 1
The 16 candidates that most likely formed in isolation.
| Star | Aliases | α(2000) | δ(2000) | RVstar | RVISM | mV | Spectral type | Mstar | Mcl | Grade |
| VFTS | [ ] |
[] |
[M⊙] | [M⊙] | ||||||
|
|
||||||||||
| 089 | ST 1-25 | 05 37 36.87 | −69 08 22.82 | 280.1 ± 0.8 | 270.6 ± 2.4 | 16.08 | O6.5 V((f))z | 33 | 660 | 1 |
| 123† | – | 05 37 42.45 | −69 12 21.58 | 270.7 ± 0.9 | 270.6 ± 1.1 | 15.78 | O6.5 Vz | 33 | 660 | 1 |
| 208 | ST 1-93 | 05 37 56.23 | −69 11 50.90 | 270.2 ± 1.0 | 275.6 ± 1.7 | 14.65 | O6 (n)fp | 46 | 1060 | 3 |
| 216 | ST 1-97 | 05 37 59.06 | −69 11 56.83 | 269.4 ± 0.5 | 274.0 ± 0.6 | 14.41 | O4 V((fc)) | 53 | 1350 | 2 |
| 382† | S 226 | 05 38 32.28 | −69 05 44.57 | 278.3 ± 1.0 | 264.4 ± 8.8 | 15.88 | O4-5 V((fc))z | 48 | 1130 | 1 |
| 385 | P 288, S 84 | 05 38 32.32 | −69 05 23.87 | 270.8 ± 0.6 | 281.3 ± 0.9 | 14.65 | O4-5 V((n))((fc)) | 48 | 1130 | 2 |
| 392 | S 268 | 05 38 32.83 | −69 05 44.60 | 278.3 ± 1.0 | 282.1 ± 1.4 | 16.10 | O6-7 V((f))z | 33 | 660 | 1 |
| 398 | Mk 59, P 341 | 05 38 33.38 | −69 04 38.39 | 268.8 ± 0.5 | 274.1 ± 0.8 | 14.40 | O5.5 V((n))((f))z | 40 | 860 | 1 |
| 470 | P 716 | 05 38 39.49 | −69 04 38.64 | 265.0 ± 1.2 | 278.3 ± 3.4 | 15.46 | O6-7 V((f))z | 33 | 660 | 1 |
| 488 | P 791 | 05 38 40.72 | −69 08 24.90 | 270.1 ± 1.0 | 268.0 ± 2.2 | 15.87 | O6 V((f))z | 36 | 740 | 1 |
| 537 | P 1022 | 05 38 43.02 | −69 03 44.78 | 271.0 ± 1.1 | 259.7 ± 1.5 | 15.99 | O5 V((fc))z | 44 | 990 | 1 |
| 577† | P 1189 | 05 38 44.94 | −69 07 04.59 | 264.5 ± 1.3 | 271.4 ± 2.8 | 16.64 | O6 V((fc))z | 36 | 740 | 1 |
| 581 | P 1218 | 05 38 45.07 | −69 04 15.57 | 277.6 ± 1.0 | 259.1 ± 3.8 | 16.07 | O4-5 V((fc)) | 48 | 1130 | 2 |
| 682*† | P 1732 | 05 38 55.51 | −69 04 26.72 | 300.0 ± 10.0 | 259.5 ± 3.0 | 16.08 | WN5h | >100 | >3900 | 1 |
| 706 | P 1838 | 05 38 58.76 | −69 05 23.93 | 269.8 ± 3.6 | 290.7 ± 0.6 | 15.77 | O6-7 Vnnz | 33 | 660 | 1 |
| 849† | – | 05 39 47.36 | −68 59 21.99 | 260.6 ± 0.8 | 262.5 ± 1.3 | 15.14 | O7 Vz | 30 | 580 | 1 |
Notes. Positions and magnitudes come from Evans et al. (2011). Eleven of the 16 candidates are Vz stars, thought to be zero-age main sequence stars (ZAMS). The final column reflects the potential ages of the candidates on the basis of their spectral types and results from Weidner & Vink (2010). Grade 1 candidates are most likely 2 Myr old or younger, grade 2 are between 2 and 4 Myr, and grade 3 are those older than 4 Myr. The values for Mcl are derived using the mmax − Mcl relationship from Weidner et al. (2010). Errors provided for the radial velocity are uncertainties from the mean. Candidates VFTS 208 and 385 show slight indications of variability, but it does not affect the current results.
The source is a Wolf-Rayet star and does not fit all criteria in Sect. 3.1. For further details see Sect. 4.1.4 and Bestenlehner et al. (2011).
References. Aliases/previous identifications of the VFTS candidates are given in the second column. The sources of identification are: Mk (Melnick 1985), P (Parker 1993), S (Selman et al. 1999) and ST (Schild & Testor 1992).
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