Table 3
Determined frequencies and suggested spherical degree l of the corresponding pulsation mode.
| SBL98 | Type | f 1 | l 1 | f 2 | l 2 | f 3 | l 3 | f 4 | f 5 | f 6 | A V, f 1 | Comment |
| ID | (d-1) | (d-1) | (d-1) | (d-1) | (d-1) | (d-1) | (mmag) | |||||
|
|
||||||||||||
| 164 | SPB | 1.4183 | 3 | 19.5 | new | |||||||
| 210 | SPB | 0.9615 | 2 | 0.8332 | 0.5004 | 1.9223 | 28.4 | f4 = 2f1, new | ||||
| 226 | β Cephei | 0.7017 | 14.9098 | 2.4242 | 2.6579 | 17.2502 | 7.5 | hybrid? | ||||
| 268 | β Cephei | 8.3847 | 12.9891 | 7.2748 | 4.7 | |||||||
| 275 | SPB | 1.6686 | 1.7662 | 0.9093 | 2.0437 | 13.0 | ||||||
| 283 | SPB | 1.6694 | 1 | 0.249 | 1.4688 | 2.9952 | 11.3 | new | ||||
| 303 | β Cephei | 10.1225 | 10.991 | 10.5106 | 4 | 11.6904 | 12.045 | 11.902 | 11.1 | |||
| 317 | SPB | 0.6133 | 1.3381 | 3.4903 | 4.9252 | 7.9 | new | |||||
| 437 | β Cephei | 7.461 | 2.0 | candidate | ||||||||
| 456 | β Cephei | 12.6701 | 2.0 | candidate | ||||||||
| 461 | SPB | 0.3597 | 1 | 4.4 | ||||||||
| 480 | SPB | 2.2981 | 4.5224 | 4.2 | new, candidate | |||||||
| 482 | SPB | 1.9461 | 1.3466 | 1,3 | 7.4 | new | ||||||
| 486 | β Cephei | 11.3791 | 13.8258 | 18.058 | (0.38) | 2.1 | ||||||
| 515 | β Cephei | 3.5221 | 5.162 | 4.0 | candidate | |||||||
| 528 | SPB | 1.1959 | 0.8962 | 1.3335 | 12.7 | new | ||||||
| 653 | β Cephei | 9.2647 | 0 | 13.334 | 4.5 | |||||||
| 712 | β Cephei | 9.8481 | 9.2947 | 5.7 | ||||||||
|
|
||||||||||||
| 306 | δ Scuti | 23.7713 | 9.4853 | 20.3195 | 9.7797 | 10.5421 | 8.9 | |||||
| 455 | δ Scuti | 23.7651 | 19.8906 | 20.869 | 18.4495 | 10.0 | ||||||
| 464 | SPB | 1.1001 | 1.3389 | 4.7 | new | |||||||
|
|
||||||||||||
| 444 | δ Scuti | 15.0539 | 20.8483 | 17.9737 | 23.0557 | 2.3 | new | |||||
| 612 | δ Scuti | 11.1654 | 10.7018 | 10.4427 | 9.2525 | 11.5 | ||||||
| 752 | δ Scuti | 15.2413 | 15.3989 | 17.1006 | 15.0161 | 18.7892 | 2.7 | new | ||||
Notes. Only stars where frequency analysis resulted in at least one significant signal are listed. The frequencies are sorted by decreasing S/N and all possible pulsation modes according to our analysis are listed. The AV,f1 column lists the amplitude of the frequency in the V band with largest S/N, i.e. f1. The first horizontal line in the list separates the confirmed members of NGC 6231 (above) from possible member stars and targets below the second horizontal line represent non-members. Typical errors are of the order of a few 10-4d-1 for the frequencies and about 0.2mmag for the V band amplitude. More detailed error estimates will be given in Appendix A where each star is discussed individually.
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