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 \sim a ^ { -3.5 } .
This model exhibits a dust-to-star luminosity ratio of 4.6 \pm 0.4 \times 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 .