  Planets have been detected in circumbinary orbits in several different
systems, despite the additional challenges faced during their formation in such
an environment. We investigate the possibility of planetary formation in the
spectroscopic binary CS Cha by analyzing its circumbinary disk. The system was
studied with high angular resolution ALMA observations at 0.87mm. Visibilities
modeling and Keplerian fitting are used to constrain the physical properties of
CS Cha, and the observations were compared to hydrodynamic simulations. Our
observations are able to resolve the disk cavity in the dust continuum emission
and the 12CO J:3-2 transition. We find the dust continuum disk to be
azimuthally axisymmetric (less than 9% of intensity variation along the ring)
and of low eccentricity (of 0.039 at the peak brightness of the ring). Under
certain conditions, low eccentricities can be achieved in simulated disks
without the need of a planet, however, the combination of low eccentricity and
axisymmetry is consistent with the presence of a Saturn-like planet orbiting
near the edge of the cavity.
