Table 13.
Fourier analysis of the residual MOST LC (from Fig. 18).
| Frequency | Period | Amplitude | Notes | |
|---|---|---|---|---|
| [c d−1] | [d] | [mmag] | ||
| f1 | 0.218 | 4.572 | 6.37 | Rotation of Aa1 |
| f2 | 0.478 | 2.090 | 3.39 | Rotation of Ab |
| f3 | 0.396 | 2.522 | 4.04 | Pulsation? |
| f4 | 0.929 | 1.075 | 3.05 | Pulsation? |
| f5 | 0.168 | 5.931 | 2.95 | Orbital (Aa1+Aa2) |
| f6 | 1.168 | 0.855 | 1.95 | Orbital + 1 c d−1 |
| f7 | 0.975 | 1.025 | 1.96 | approx. 1 c d−1 |
| f8 | 0.346 | 2.887 | 2.54 | 2forb? |
| f9 | 0.086 | 11.551 | 1.67 | 0.5forb? |
| f10 | 2.214 | 0.451 | 1.29 | Pulsation? |
Notes. The synthetic LC was subtracted and eclipses were removed to suppress the binary signal. The first two frequencies are then identified as the rotation frequency of the primary (Aa1; Nichols et al. 2015) and the tertiary (Ab; this work). The uncertainty is determined by the time span, fΔ = 0.045 c d−1. For reference, the orbital frequency of the Aa1+Aa2 binary forb = 0.174 c d−1, and the orbital frequency of the satellite fmost = 14.19 c d−1.
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