Table 5.
BPM 31594: Results of the fit of the data set derived from the ultrashort cadence mode TESS observations (‘This work’).
| This work |
P01 – Bognár et al. (2020) |
||||||
|---|---|---|---|---|---|---|---|
| Frequency [μHz] | Period [s] | Amplitude [mma] | Frequency [μHz] | Period [s] | Amplitude [mma] | Sel. | |
| Δ | 13.409(12) | 74577 | 3.08(32) | ||||
| 871.799(18) | 1147.053 | 1.45(24) | 0.54f4 | ||||
| 877.261(18) | 1139.912 | 1.46(24) | f1 | x | |||
| 1460.726(17) | 684.591 | 1.58(26) | f2 | 1461.117(13) | 684.408 | 2.87(32) | x |
| 1548.328(7) | 645.858 | 3.70(26) | f3 | 1548.455(4) | 645.805 | 8.47(32) | x |
| 1605.950(3)+ | 622.684 | 8.68(27) | f4 − Δ | 1604.982(4) | 623.060 | 8.94(32) | |
| 1618.374(1)+ | 617.904 | 32.44(27) | f4 | 1618.401(1) | 617.894 | 39.37(32) | x |
| 1630.778(3)+ | 613.204 | 8.50(27) | f4 + Δ | 1631.844(4) | 612.804 | 10.80(32) | |
| 2483.254(4) | 402.697 | 6.40(30) | fx | 2483.203(7) | 402.706 | 5.06(32) | |
| 2490.171(5)+ | 401.579 | 6.09(30) | 1.54f4 | 2490.147(7) | 401.582 | 5.35(32) | |
| 3166.716(12) | 315.785 | 2.40(32) | f3 + f4 | 3166.877(9) | 315.769 | 4.05(32) | |
| 3224.310(13) | 310.144 | 2.15(32) | 2f4 − Δ | ||||
| 3236.751(4)+ | 308.952 | 7.21(33) | 2f4 | 3236.794(6) | 308.948 | 6.26(32) | |
| 3245.653(6) | 308.104 | 4.85(32) | fy | 3245.648(11) | 308.105 | 3.41(32) | |
| 3249.136(12)+ | 307.774 | 2.26(32) | 2f4 + Δ | ||||
| 3252.603(7) | 307.446 | 4.24(32) | fw | 3252.590(12) | 307.447 | 3.16(32) | |
| 4108.546(12)+ | 243.395 | 2.51(35) | 2.54f4 | 4108.584(15) | 243.393 | 2.49(32) | |
| 4114.021(12) | 243.071 | 2.34(35) | fz | 4115.083(16) | 243.009 | 2.41(32) | |
| 4855.098(9)+ | 205.969 | 2.55(37) | 3f4 | ||||
| 5726.912(18) | 174.614 | 1.74(39) | 3.54f4 | ||||
Notes. We use plus symbols to mark where closely spaced peaks around a larger-amplitude one exist. These may not represent additional independent pulsational frequencies, and therefore we do not include them in this list. The errors are formal uncertainties. We also present a possible frequency identification in the fourth column. We use an ‘x’ to mark the frequencies selected for asteroseismic period fits.
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