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94 Ceti is a triple star system with a circumprimary gas giant planet andfar-infrared excess. Such excesses around main sequence stars are likely due todebris discs, and are considered as signposts of planetary systems and,therefore, provide important insights into the configuration and evolution ofthe planetary system. Consequently, in order to learn more about the 94 Cetisystem, we aim to precisely model the dust emission to fit its observed SED andto simulate its orbital dynamics. We interpret our APEX bolometric observationsand complement them with archived Spitzer and Herschel bolometric data toexplore the stellar excess and to map out background sources in the fields.Dynamical simulations and 3D radiative transfer calculations were used toconstrain the debris disc configurations and model the dust emission. The bestfit dust disc model for 94 Ceti implies a circumbinary disc around thesecondary pair, limited by dynamics to radii smaller than 40 AU and with agrain size power-law distribution of ~a^-3.5. This model exhibits adust-to-star luminosity ratio of 4.6+-0.4*10^-6. The system is dynamicallystable and N-body symplectic simulations results are consistent withsemi-analytical equations that describe orbits in binary systems. In theobservations we also find tentative evidence of a circumtertiary ring thatcould be edge-on.

94 Ceti: a triple star with a planet and dust disc