Table A.3.
Number of possible isolated stars relative to nearby clusters or OB associations (solar metallicity and SMC-like extinction law setup)
| Sample | Method 1 | Method 2 | ||
|---|---|---|---|---|
| dthresh, 1 = 74pc | Number | Frequency | Number | Frequency |
| only clusters | ||||
| D.O.F. = 4 | 70 | 0.298 | 70 | 0.298 |
| D.O.F. = 3 | 87 | 0.370 | 91 | 0.387 |
| D.O.F. = 2 | 19 | 0.081 | 20 | 0.085 |
| whole sample | 176 | 0.749 | 181 | 0.770 |
| only OB associations | ||||
| D.O.F. = 4 | 81 | 0.345 | 83 | 0.353 |
| D.O.F. = 3 | 93 | 0.396 | 95 | 0.404 |
| D.O.F. = 2 | 15 | 0.064 | 16 | 0.068 |
| whole sample | 189 | 0.804 | 194 | 0.826 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 66 | 0.281 | 66 | 0.281 |
| D.O.F. = 3 | 81 | 0.345 | 86 | 0.366 |
| D.O.F. = 2 | 13 | 0.055 | 15 | 0.064 |
| whole sample | 160 | 0.681 | 167 | 0.711 |
| dthresh, 2 = 204pc | Number | Frequency | Number | Frequency |
| only clusters | ||||
| D.O.F. = 4 | 35 | 0.149 | 41 | 0.174 |
| D.O.F. = 3 | 58 | 0.247 | 70 | 0.298 |
| D.O.F. = 2 | 9 | 0.038 | 11 | 0.047 |
| whole sample | 102 | 0.434 | 122 | 0.519 |
| only OB associations | ||||
| D.O.F. = 4 | 64 | 0.272 | 68 | 0.289 |
| D.O.F. = 3 | 85 | 0.362 | 91 | 0.387 |
| D.O.F. = 2 | 11 | 0.047 | 13 | 0.055 |
| whole sample | 160 | 0.681 | 172 | 0.732 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 26 | 0.111 | 33 | 0.140 |
| D.O.F. = 3 | 50 | 0.213 | 64 | 0.272 |
| D.O.F. = 2 | 4 | 0.17 | 8 | 0.034 |
| whole sample | 80 | 0.340 | 105 | 0.447 |
Notes. Number and frequency of possible isolated stars relative to nearby 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 235 using a solar metallicity and an SMC-like extinction law.
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