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Table 2.
Optimised parameters for the extracted red noise (cf. Eq. (1)) for the stars studied in this paper using our Bayesian MCMC method, and the dominant cause(s) that are likely contributing to the observed low-frequency power excess, which are not only sourced from this work but also from the literature.
| Name | α0 | νchar | γ | PW | Var. Type |
|---|---|---|---|---|---|
| (ppm2/μHz) | (μHz) | (ppm2/μHz) | |||
| O stars from Blomme et al. (2011) inferred to have IGWs by Aerts & Rogers (2015): | |||||
| HD 46150 | 49205.559 ± 0.087 | 24.120096 ± 0.000072 | 1.8777210 ± 0.0000052 | 7.073 ± 0.002 | puls + wind |
| HD 46223 | 160242.358 ± 0.088 | 17.742474 ± 0.000015 | 1.8082826 ± 0.0000014 | 22.921 ± 0.002 | puls + wind |
| HD 46966 | 18249.642 ± 0.069 | 30.072804 ± 0.000161 | 2.1927641 ± 0.0000155 | 12.602 ± 0.003 | puls + wind |
| CoRoT OBAF stars with detected stochastic low-frequency variability: | |||||
| HD 45418 | 3203.510 ± 0.034 | 30.607811 ± 0.000361 | 4.8896087 ± 0.0001728 | 5.590 ± 0.001 | puls |
| HD 45517 | 327.068 ± 0.067 | 10.209637 ± 0.002210 | 4.0164748 ± 0.0025992 | 8.393 ± 0.001 | puls |
| HD 45546 | 34626.797 ± 0.054 | 24.157404 ± 0.000046 | 3.2662493 ± 0.0000125 | 9.865 ± 0.001 | puls |
| HD 46149 | 4994.164 ± 0.065 | 13.545526 ± 0.000147 | 6.5129408 ± 0.0004626 | 8.270 ± 0.002 | puls + wind |
| HD 46179 | 21.717 ± 0.089 | 15.161279 ± 0.084005 | 2.2933918 ± 0.0167594 | 1.987 ± 0.001 | puls |
| HD 46202 | 537.336 ± 0.059 | 31.854515 ± 0.004408 | 3.0236231 ± 0.0008187 | 7.858 ± 0.002 | puls + wind |
| HD 46769 | 35.278 ± 0.074 | 23.411051 ± 0.068442 | 2.1318523 ± 0.0090258 | 0.908 ± 0.002 | gran |
| HD 48784 | 2299.504 ± 0.056 | 30.020785 ± 0.000762 | 4.0222079 ± 0.0003455 | 3.192 ± 0.002 | gran + puls |
| HD 49677 | 246.504 ± 0.117 | 11.178924 ± 0.006973 | 2.2987365 ± 0.0016031 | 6.888 ± 0.002 | puls |
| HD 50747 | 2840.821 ± 0.052 | 44.340794 ± 0.001147 | 3.3346001 ± 0.0002550 | 1.077 ± 0.001 | puls |
| HD 51332 | 757.890 ± 0.087 | 18.108611 ± 0.003225 | 1.9357792 ± 0.0003633 | 3.745 ± 0.001 | puls + gran |
| HD 51756 | 6458.932 ± 0.060 | 24.569608 ± 0.000341 | 2.2164263 ± 0.0000373 | 4.888 ± 0.001 | puls + wind |
| HD 52130 | 2320.871 ± 0.029 | 43.503073 ± 0.000515 | 5.3152045 ± 0.0002527 | 21.266 ± 0.001 | puls + gran |
| HD 174589 | 1856.345 ± 0.179 | 8.984878 ± 0.001486 | 1.4239502 ± 0.0001289 | 2.688 ± 0.002 | puls + gran |
| HD 174966 | 401.056 ± 0.101 | 33.149762 ± 0.016483 | 1.2198259 ± 0.0002660 | 4.006 ± 0.003 | puls + gran |
| HD 174967 | 404.584 ± 0.074 | 15.102132 ± 0.002910 | 4.2063454 ± 0.0027710 | 32.480 ± 0.002 | puls |
| HD 174990 | 341.897 ± 0.059 | 24.196653 ± 0.004067 | 5.9565225 ± 0.0042772 | 17.059 ± 0.002 | puls |
| HD 175272 | 884.411 ± 0.135 | 10.357587 ± 0.002366 | 2.0133028 ± 0.0004521 | 3.792 ± 0.002 | puls |
| HD 175542 | 147.397 ± 0.073 | 31.671226 ± 0.019787 | 2.6875427 ± 0.0030297 | 17.831 ± 0.006 | puls |
| HD 175640 | 23.213 ± 0.071 | 35.170619 ± 0.134604 | 2.8834658 ± 0.0219825 | 1.496 ± 0.006 | puls |
| HD 263425 | 3155.639 ± 0.535 | 3.267273 ± 0.000919 | 1.2824296 ± 0.0001254 | 25.100 ± 0.002 | puls |
| Additional OBAF stars with insufficient CoRoT data for an accurate background fit: | |||||
| HD 47485 | 31438.683 ± 0.021 | 125.735343 ± 0.000056 | 12.2180879 ± 0.0000552 | 56.380 ± 0.002 | gran + puls |
| HD 48977 | 30314.154 ± 0.064 | 34.301079 ± 0.000087 | 3.2625348 ± 0.0000179 | 7.380 ± 0.002 | puls + wind |
| HD 50844 | 33248.802 ± 0.011 | 257.800434 ± 0.000072 | 6.6387810 ± 0.0000101 | 57.262 ± 0.001 | gran + puls |
| HD 50870 | 4513.878 ± 0.009 | 354.121974 ± 0.000514 | 10.1627352 ± 0.0001001 | 28.953 ± 0.001 | gran + puls |
| HD 51193 | 554739.578 ± 0.053 | 25.007251 ± 0.000007 | 3.0604732 ± 0.0000007 | 88.077 ± 0.001 | puls |
| HD 51452 | 880984.219 ± 0.054 | 23.579036 ± 0.000002 | 3.1299536 ± 0.0000005 | 144.210 ± 0.001 | puls + wind |
| HD 51359 | 2200.012 ± 0.009 | 303.217065 ± 0.000859 | 14.3801743 ± 0.0003426 | 10.686 ± 0.001 | gran + puls |
| HD 51722 | 8629.083 ± 0.013 | 225.375146 ± 0.000292 | 6.2225653 ± 0.0000433 | 11.397 ± 0.001 | gran + puls |
| HD 174532 | 1941.594 ± 0.012 | 402.953130 ± 0.001633 | 13.9727879 ± 0.0005824 | 9.410 ± 0.002 | gran + puls |
| HD 174936 | 625.629 ± 0.011 | 628.365922 ± 0.005419 | 17.0182510 ± 0.0018970 | 25.638 ± 0.006 | gran + puls |
| HD 175445 | 280.216 ± 0.026 | 279.849349 ± 0.025642 | 3.6303503 ± 0.0010499 | 4.030 ± 0.008 | puls + gran |
Notes. We note that pulsation can refer to coherent modes and/or damped modes (i.e. IGWs).
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