Table 3
Number of stars around each candidate based on observations and Monte Carlo stellar cluster simulations.
| VFTS | NNinner | NNfield | Nexcess | Nsim |
| [stars pc-2] | [stars pc-2] | [star count] | [star count] | |
|
|
||||
| 089 | 0.09 | 0.07 | 2 | 53 |
| 123 | 2.01 | 2.23 | −17 | 53 |
| 208 | 2.93 | 2.61 | 25 | 53 |
| 216 | 2.67 | 2.51 | 13 | 53 |
| 382 | 0.32 | 0.22 | 7 | 53 |
| 385 | 0.32 | 0.38 | −5 | 53 |
| 392 | 0.35 | 0.22 | 11 | 53 |
| 398 | 0.37 | 0.46 | −7 | 53 |
| 470 | 0.51 | 0.48 | 3 | 53 |
| 488 | 0.64 | 0.39 | 19 | 53 |
| 537 | 0.22 | 0.29 | −6 | 53 |
| 577 | 0.70 | 0.66 | 3 | 53 |
| 581 | 0.31 | 0.41 | −9 | 53 |
| 682 | 0.05 | 0.07 | −2 | 148 |
| 706 | 0.22 | 0.12 | 8 | 53 |
| 849 | 0.28 | 0.19 | 7 | 11 |
Notes. If the mmax − Mcl relationship is correct we should see an excess number of stars within a 5 pc radius of each of the candidates. Around each candidate we measured the number of observable stars above 3 M⊙ from the HST images and compared the number of excess sources (Nexcess) to the Monte Carlo simulations (Nsim). This shows no evidence of clustering around the massive star candidates.
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