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Wide low-mass substellar companions are known to be very rare among low-massstars, but appear to become increasingly common with increasing stellar mass.However, B-type stars, which are the most massive stars within ~150 pc of theSun, have not yet been examined to the same extent as AFGKM-type stars in thatregard. In order to address this issue, we launched the ongoing B-starExoplanet Abundance Study (BEAST) to examine the frequency and properties ofplanets, brown dwarfs, and disks around B-type stars in the Scorpius-Centaurus(Sco-Cen) association; we also analyzed archival data of B-type stars inSco-Cen. During this process, we identified a candidate substellar companion tothe B9-type spectroscopic binary HIP 79098 AB, which we refer to as HIP 79098(AB)b. The candidate had been previously reported in the literature, but wasclassified as a background contaminant on the basis of its peculiar colors.Here we demonstrate that the colors of HIP 79098 (AB)b are consistent withseveral recently discovered young and low-mass brown dwarfs, including othercompanions to stars in Sco-Cen. Furthermore, we show unambiguous common propermotion over a 15-year baseline, robustly identifying HIP 79098 (AB)b as a bonafide substellar circumbinary companion at a 345+/-6 AU projected separation tothe B9-type stellar pair. With a model-dependent mass of 16-25 Mjup yielding amass ratio of <1%, HIP 79098 (AB)b joins a growing number of substellarcompanions with planet-like mass ratios around massive stars. Our observationsunderline the importance of common proper motion analysis in the identificationof physical companionship, and imply that additional companions couldpotentially remain hidden in the archives of purely photometric surveys.

The B-Star Exoplanet Abundance Study: a co-moving 16-25 Mjup companion to the young binary system HIP 79098