Table A.5.
Number of possible isolated stars relative to nearby clusters or OB associations (SMC-like 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 | 93 | 0.304 | 98 | 0.320 |
| D.O.F. = 3 | 117 | 0.382 | 126 | 0.412 |
| D.O.F. = 2 | 23 | 0.075 | 23 | 0.075 |
| whole sample | 233 | 0.761 | 247 | 0.807 |
| only OB associations | ||||
| D.O.F. = 4 | 111 | 0.363 | 117 | 0.382 |
| D.O.F. = 3 | 128 | 0.418 | 133 | 0.435 |
| D.O.F. = 2 | 18 | 0.059 | 20 | 0.065 |
| whole sample | 257 | 0.840 | 270 | 0.882 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 89 | 0.291 | 94 | 0.307 |
| D.O.F. = 3 | 112 | 0.366 | 122 | 0.399 |
| D.O.F. = 2 | 16 | 0.052 | 18 | 0.059 |
| whole sample | 217 | 0.709 | 234 | 0.765 |
| dthresh, 2 = 204pc | Number | Frequency | Number | Frequency |
| only clusters | ||||
| D.O.F. = 4 | 44 | 0.144 | 52 | 0.170 |
| D.O.F. = 3 | 74 | 0.242 | 93 | 0.304 |
| D.O.F. = 2 | 12 | 0.039 | 14 | 0.046 |
| whole sample | 130 | 0.425 | 159 | 0.520 |
| only OB associations | ||||
| D.O.F. = 4 | 89 | 0.291 | 100 | 0.327 |
| D.O.F. = 3 | 117 | 0.382 | 127 | 0.415 |
| D.O.F. = 2 | 13 | 0.042 | 16 | 0.052 |
| whole sample | 219 | 0.716 | 243 | 0.794 |
| clusters + OB associations | ||||
| D.O.F. = 4 | 34 | 0.111 | 43 | 0.141 |
| D.O.F. = 3 | 65 | 0.212 | 85 | 0.278 |
| D.O.F. = 2 | 6 | 0.020 | 10 | 0.033 |
| whole sample | 105 | 0.343 | 138 | 0.451 |
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 306 using an SMC-like metallicity and an SMC-like extinction law.
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