Fig. 3: Diagrams showing the mass of companions (in M⊙) that may be responsible for the observed Proper Motion anomaly (PMA)55 as a function of semi-major axis a in au (blue solid line).
From: Jupiter-like planets might be common in a low-density environment
They are compared with 90% confidence upper limits obtained from the Gaia RUWE parameter (green dashed line), the upper limit from high-contrast imaging (HCI) with SPHERE30 (orange solid line), and the upper limit from RVs (red dotted line)109. The solid violet lines mark the position of known debris disks78 and the dash-dotted violet lines are the outer edge of the stability region due to the presence of these disks or of known companion (HIP 10679). Upper left panel: HIP 560, HCI from Dahlqvist et al.106; Upper right panel: HIP 10679, HCI from Dahlqvist et al.106; Lower left panel: HIP 84586 HCI from Asensio-Torres et al.104; Lower right panel: HIP 88399, HCI from Mesa et al.103. The orange area is occupied by Jupiter-like planets. The companions responsible for the PMa should be close to the solid blue line, below the dashed green, the solid orange line, the dotted red line, and the left of the dash-dotted violet line.
