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We carry out three dimensional smoothed particle hydrodynamics simulations tostudy the impact of planet-disc interactions on a gravitationally unstableprotoplanetary disc. We find that the impact of a planet on the disc'sevolution can be described by three scenarios. If the planet is sufficientlymassive, the spiral wakes generated by the planet dominate the evolution of thedisc and gravitational instabilities are completely suppressed. If the planet'smass is too small, then gravitational instabilities are unaffected. If theplanet's mass lies between these extremes, gravitational instabilities areweakened. We present mock Atacama Large Millimeter/submillimeter Array (ALMA)continuum observations showing that the observability of large-scale spiralstructures is diminished or completely suppressed when the planet is massiveenough to influence the disc's evolution. Our results show that massive discsthat would be expected to be gravitationally unstable can appear axisymmetricin the presence of a planet. Thus, the absence of observed large-scale spiralstructures alone is not enough to place upper limits on the disc's mass, whichcould have implications on observations of young Class I discs with rings &gaps.

Continuing to Hide Signatures of Gravitational Instability in Protoplanetary Discs with Planets