  We test the hypothesis that an embedded giant planet in the IM Lupi
protostellar disc can produce velocity kinks seen in CO line observations as
well as the spiral arms seen in scattered light and continuum emission. We
inject planets into 3D hydrodynamics simulations of IM Lupi, generating
synthetic observations using Monte Carlo radiative transfer. We find that an
embedded planet of 2-3 times the mass of Jupiter can reproduce non-Keplerian
velocity perturbations, or `kinks', in the 12CO J=2-1 channel maps. Such a
planet can also explain the spiral arms seen in 1.25mm dust continuum emission
and 1.6 micron scattered light images. We show that the wake of the planet can
be traced in the observed peak velocity map, which appears to closely follow
the morphology expected from our simulations and from analytic models of
planet-disc interaction.
