Fig. 1: Orbital separation and mass of a companion that could produce the Gaia proper motion anomaly of MP Mus.
From: A young gas giant and hidden substructures in a protoplanetary disk
Left: the individual Gaia simulations that produce an astrometric signal compatible with the observations (0.26 > ∣Δμ∣ > 0.16 mas yr−1, ∣Δμ∣/σ∣Δμ∣ > 4 and UWEDR3 <1.1). Right: the same simulations but smoothed over a two-dimensional histogram (contours correspond to 0.05%, 0.15% and 0.2%). When considering the disk structure traced in the millimetre (shaded area), the most likely companion is a gas giant at 1–2 au. Crosses indicate the parameters used for the hydrodynamical simulations in the ‘Confronting observations with simulations’ section. The simulations that best reproduce both Gaia and ALMA observations are shown in red (Discussion).
