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Table A.1.

Overview of the most prominent aliases for each star.

δ Cep

No. Frequency [d−1] Period [d] Identification
a0 0.1707315(2) 5.8571492 fF − fW
a1 0.2019469(2) 4.9517959 fF + fW
a2 0.6272367(2) 1.5942945 1 − f2

BG Cru

a0 0.22251311(3) 2.84258162 (1 − fX)/3
a1 0.35179289(3) 2.84258162 (1 − f1O)/2
a2 0.4044671(3) 2.47238898 1 − 2f0
a3 0.44502623(3) 2.84258162 2(1 − fX)/3 = 2a0
a4 0.50070001(3) 1.99720388 (1 − fLF)/2 = a10/2
a5 0.65095304(3) 1.53620912 (1 + f1O)/2
a6 0.67034645(3) 1.49176593 1 − fX
a7 0.70362726(3) 1.42120703 1 − f1O
a8 0.83515493(3) 1.19738262 1 − f4
a9 0.96947046(3) 1.03149094 1 − f0
a10 1.00098330(3) 0.99901766 1 − fLF
a11 1.03601635(3) 0.96523573 1 + f0

X Sgr

a0 0.38815911(4) 2.57626314 (1 − f1)/2
a1 0.61193616(4) 1.63415740 (1 + f1)/2
a2 0.77626756(4) 1.28821562 1 − f1
a3 0.85749957(4) 1.16618135 1 − fFU
a4 0.88947883(4) 1.12425385 1 − f0
a5 0.92153591(4) 1.08514491 1 − fX

Notes. The window periodogram analysis reveals dominant signals at 1 d−1 and 2 d−1 for all stars, with the exception of δ Cep, where the second most prominent signal is detected at fW = 0.016 d−1.

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