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We investigate the minimum planet mass that produces observable signatures ininfrared scattered light and submm continuum images and demonstrate how theseimages can be used to measure planet masses to within a factor of about two. Tothis end we perform multi-fluid gas and dust simulations of discs containinglow mass planets, generating simulated observations at $1.65 \mu$m, $10 \mu$mand $850 \mu$m. We show that the minimum planet mass that produces a detectablesignature is $\sim 15 M_\oplus$: this value is strongly dependent on disctemperature and changes slightly with wavelength (favouring the submm). We alsoconfirm previous results that there is a minimum planet mass of $\sim 20M_\oplus$ that produces a pressure maximum in the disc: only planets above thisthreshold mass generate a dust trap that can eventually create a hole in thesubmm dust. Below this mass, planets produce annular enhancements in dustoutward of the planet and a reduction in the vicinity of the planet. Thesefeatures are in steady state and can be understood in terms of variations inthe dust radial velocity, imposed by the perturbed gas pressure radial profile,analogous to a traffic jam. We also show how planet masses can be derived fromstructure in scattered light and sub-mm images. We emphasise that simulationswith dust need to be run over thousands of planetary orbits so as to allow thegas profile to achieve a steady state and caution against the estimation ofplanet masses using gas only simulations.

The minimum mass of detectable planets in protoplanetary discs and the derivation of planetary masses from high resolution observations