Observational signatures of eccentric Jupiters inside gas cavities in protoplanetary discs

Predicting how a young planet shapes the gas and dust emission of its parent disc is key to constraining presence unseen planets in protoplanetary observations. We investigate case 2 Jupiter mass that becomes eccentric after migrating into low-density cavity disc. Two-dimensional hydrodynamical simulations are performed post-processed by three-dimensional radiative transfer calculations. In our model, eccentricity reaches ~0.25, which induces strong asymmetries density inside cavity. These enhanced photodissociation form large-scale 12CO J=3-2 integrated intensity maps. They shown be detectable for an angular resolution noise level similar those achieved ALMA Furthermore, renders eccentric, manifests as narrowing, stretching twisting iso-velocity contours velocity maps J=3-2. The does not, however, give rise signatures 13CO C18O because low column densities. Outside cavity, maintains near-circular orbits, vertically extended optically thick CO displays four-lobed pattern inclinations > 30 degrees. lack large small model further implies synthetic images continuum sub-millimetre, polarized scattered light near-infrared, do not show significant differences when or still circular