Table A.1.
Number of possible isolated stars relative to nearby clusters or OB associations (SMC-like metallicity and MW-like extinction law setup)
| Sample | Method 1 | Method 2 | ||
|---|---|---|---|---|
| dthresh, 1 = 74pc | Number | Frequency | Number | Frequency |
| only clusters | ||||
| D.O.F = 4 | 93 | 0.304 | 104 | 0.340 |
| D.O.F. = 3 | 117 | 0.382 | 123 | 0.402 |
| D.O.F. = 2 | 23 | 0.075 | 23 | 0.075 |
| whole sample | 233 | 0.761 | 250 | 0.817 |
| only OB associations | ||||
| D.O.F. = 4 | 111 | 0.363 | 121 | 0.395 |
| D.O.F. = 3 | 128 | 0.418 | 133 | 0.435 |
| D.O.F. = 2 | 18 | 0.059 | 21 | 0.069 |
| whole sample | 257 | 0.840 | 275 | 0.899 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 89 | 0.291 | 102 | 0.333 |
| D.O.F. = 3 | 112 | 0.366 | 119 | 0.389 |
| D.O.F. = 2 | 16 | 0.052 | 19 | 0.062 |
| whole sample | 217 | 0.709 | 240 | 0.784 |
| dthresh, 2 = 204pc | Number | Frequency | Number | Frequency |
| only clusters | ||||
| D.O.F. = 4 | 44 | 0.144 | 59 | 0.193 |
| D.O.F. = 3 | 74 | 0.242 | 87 | 0.284 |
| D.O.F. = 2 | 12 | 0.039 | 15 | 0.049 |
| whole sample | 130 | 0.425 | 161 | 0.526 |
| only OB associations | ||||
| D.O.F. = 4 | 89 | 0.291 | 105 | 0.343 |
| D.O.F. = 3 | 117 | 0.382 | 127 | 0.415 |
| D.O.F. = 2 | 13 | 0.042 | 18 | 0.059 |
| whole sample | 219 | 0.716 | 250 | 0.817 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 34 | 0.111 | 52 | 0.170 |
| D.O.F. = 3 | 65 | 0.212 | 79 | 0.258 |
| D.O.F. = 2 | 6 | 0.020 | 13 | 0.042 |
| whole sample | 105 | 0.343 | 144 | 0.471 |
Notes. Number and frequency of possible isolated stars relative to star clusters and OB associations and given the threshold distance of dthresh, 1 = 74 pc and dthresh, 2 = 204 pc. Method 1 takes into account only the de-projected positions of stars, clusters and OB associations, while method 2 considers stellar groups whose age difference is 5 Myr at most. The number of stars is 306 using an SMC-like metallicity and a MW-like extinction law.
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