Barycentric wobble as a function of separation and mass ratio for TNO binaries with unique orbit solutions. Mass ratios are estimated under the assumption of equal albedo and equal density and are uncertain by a factor of a few (except for Eris and Haumea; M. E. Brown & B. J. Butler 2023; B. Proudfoot et al. 2024a). Binaries labeled in bold have had successful occultation detections of their companions (E. Fernández-Valenzuela et al. 2025, 2026; F. Rommel et al. 2025a, 2025b, this work). Objects above the red dashed lines present more than 20 mas in astrometric wobble.