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