http://arxiv.org/abs/2304.03607
[Abridged] The aim of this work is to identify potential signatures from planet-disc interaction in the circumstellar discs around the young stars MWC 480, HD 163296, AS 209, IM Lup, and GM Aur, through the study of molecular lines observed as part of the ALMA large program MAPS. Extended and localised perturbations in velocity, line width, and intensity have been analysed jointly using the discminer framework, in three bright CO lines, 12CO, 13CO and C18O $J=2-1$, to provide a comprehensive summary of the kinematic and column density substructures that planets might be actively sculpting in these discs. We find convincing evidence for the presence of four giant planets located at wide orbits in three of the discs in the sample: two around HD 163296, one in MWC 480, and one in AS 209. One of the planet candidates in HD 163296, P94, originally proposed by Izquierdo et al. (2022) using lower velocity resolution 12CO data, is confirmed and linked to localised velocity and line width perturbations in 13CO and C18O too. We highlight that line widths are also powerful tracers of planet-forming sites as they are sensitive to turbulent motions triggered by planet-disc interactions. In MWC 480, we identified non-axisymmetric line width enhancements around the radial separation of candidate planet-driven buoyancy spirals proposed by Teague et al. (2021), which we used to narrow the location of the planet candidate to an orbital radius of $R=245$ au and $\rm{PA}=193^\circ$. In the disc of AS 209, we found excess 12CO line widths centred at $R=210$ au, $\rm{PA}=151^\circ$, spanning around the immediate vicinity of the circumplanetary disc candidate proposed by Bae et al. (2022), which further supports its presence. Our simultaneous analysis of multiple tracers and observables aims to lay the groundwork for robust studies of molecular line properties focused on the search for young planets in discs.
A. Izquierdo, L. Testi, S. Facchini, et. al.
Mon, 10 Apr 23
13/36
Comments: Accepted for publication in A&A
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