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Recent imaging of the disc around the V4046$\,$Sgr spectroscopic binaryrevealed concentric regions of dust rings and gaps. The object's proximity andexpected equilibrated state due to its old age (>20$\,$Myr) make it a superbtestbed for hydrodynamical studies in direct comparison to observations. Weemploy two-dimensional hydrodynamical simulations of gas and multiple dustspecies to test whether the observed structure conforms with the presence ofgiant planets embedded in the disc. We then perform radiative transfercalculations of sky images, which we filter for the telescope response forcomparison with near-infrared and millimetre observations. We find that theexisting data are in excellent agreement with a flared disc and the presence oftwo giant planets, at 9$\,$au and 20$\,$au, respectively. The different ringwidths are recovered by diffusion-balanced dust trapping within the gaspressure maxima. In our radiative transfer model, the diffusion in verticaldirection is reduced in comparison to the radial value by a factor of five torecover the spectral energy distribution. Further, we report a previouslyunaddressed, azimuthally-confined intensity decrement on the bright inner ringin the near-infrared scattered light observation. Our model shows that thisdecrement can be explained by a shadow cast by a circumplanetary disc aroundthe same giant planet that creates the inner cavity in the hydrodynamicalsimulations. We examine the shape of the intensity indentation and discuss thepotential characterisation of a giant planet and its associated disc by itsprojected shadow in scattered light observations.

monthly notices of the royal astronomical society

The steady-state hydrodynamics of a long-lived disc: planetary system  architecture and prospects of observing a circumplanetary disc shadow in  V4046$\,$Sgr