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Thanks to large dedicated surveys, large-scale magnetic fields have beendetected for about 10% of early-type stars. We aim to precisely characterizethe large-scale magnetic field of the magnetic component of the wide binary $o$Lup, by using high-resolution ESPaDOnS and HARPSpol spectropolarimetry toanalyse the variability of the measured longitudinal magnetic field. Inaddition, we investigate the periodic variability using space-based photometrycollected with the BRITE-Constellation by means of iterative prewhitening. Therotational variability of the longitudinal magnetic field indicates a rotationperiod $P_{\mathrm{rot}}=2.95333(2)$d and that the large-scale magnetic fieldis dipolar, but with a significant quadrupolar contribution. Strong differencesin the strength of the measured magnetic field occur for various chemicalelements as well as rotational modulation for Fe and Si absorption lines,suggesting a inhomogeneous surface distribution of chemical elements. Estimatesof the geometry of the large-scale magnetic field indicate $i=27\pm10^{\circ}$, $\beta = 74^{+7}_{-9}\,^{\circ}$, and a polar field strength of atleast 5.25 kG. The BRITE photometry reveals the rotation frequency and severalof its harmonics, as well as two gravity mode pulsation frequencies. Thehigh-amplitude g-mode pulsation at $f=1.1057\mathrm{d^{-1}}$ dominates theline-profile variability of the majority of the spectroscopic absorption lines.We do not find direct observational evidence of the secondary in thespectroscopy. Therefore, we attribute the pulsations and the large-scalemagnetic field to the B5IV primary of the $o$ Lup system, but we discuss theimplications should the secondary contribute to or cause the observedvariability.

Magnetic characterization and variability study of the magnetic SPB star o Lup