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Table 2.

Significant periodic photometric variability seen in the UBr and BAb BRITE photometry of o Lupi.

ID Origin UBr
f δf A S/N f δf A S/N
(d−1) (10−4 d−1) (±0.17 ppt) (d−1) (10−4 d−1) (±0.35 ppt)
f1 frot 0.33869 1.5 4.63 9.6 0.33792 2.9 5.02 4.7
f2 2frot 0.67706 1.3 5.03 8.5 0.67687 3.2 4.62 5.0
f3 g mode 1.10572 0.9 7.14 10.0 1.10611 1.9 7.65 5.8
f4 finst 1.00078 3.5 1.91 5.9
f5 3frot 1.01586 5.2 1.29 4.5
f6 g mode 1.29852 4.8 1.40 4.8

Notes. We indicate the frequency and corresponding amplitude, A, together with their respective uncertainties, as well as the S/N of the detection in the Lomb-Scargle periodogram during the iterative prewhitening procedure. The frequency and amplitude uncertainties are determined from Montgomery & O’Donoghue (1999), under the assumption of white noise and uncorrelated data. These conditions are not always fullfilled and result in a typical underestimation of the frequency error by a factor 10 (e.g., Degroote et al. 2009b). We also indicate the proposed origin of the observed periodic photometric variability and remark that a more precise value for the rotation period was obtained through the magnetometric analysis in Sect. 5.

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