Kinematic evidence for an embedded planet in the IM Lupi disc

Abstract

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.

arXiv comment10 pages, 6 figures, accepted to ApJL. Radiative transfer models and a movie showing change with azimuth available from https://doi.org/10.26180/20145620.v3

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• Support for fragile porous dust in a gravitationally self-regulated disk around IM Lup
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• Kinematic and thermal signatures of the directly imaged protoplanet candidate around Elias 2-24
• A potential site for wide-orbit giant planet formation in the IM Lup disk
• Filling in the Gaps: Can Gravitationally Unstable Discs Form the Seeds of Gas Giant Planets?
• Testing velocity kinks as a planet-detection method: Do velocity kinks in surface gas emission trace planetary spiral wakes in the midplane continuum?
• Winding Motion of Spirals in a Gravitationally Unstable Protoplanetary Disk
• Gravitational instability in planet-forming discs