Robust Evidence for the Breakdown of Standard Gravity at Low Acceleration from Statistically Pure Binaries Free of Hidden Companions

Abstract

It is found that Gaia Data Release 3 binary stars selected with stringent requirements on astrometric measurements and radial velocities naturally satisfy Newtonian dynamics without hidden close companions when the projected separation s ≲ 2 kau, showing that pure binaries can be selected. It is then found that pure binaries selected with the same criteria show a systematic deviation from the Newtonian expectation when s ≳ 2 kau. When both proper motions and parallaxes are required to have precision better than 0.005 and radial velocities better than 0.2, I obtain 2463 statistically pure binaries within a “clean” G -band absolute magnitude range. From this sample, I obtain an observed-to-Newtonian predicted kinematic acceleration ratio of γ g = g obs / g pred = 1.49 − 0.19 + 0.21 for acceleration ≲10 −10 m s −2 , in excellent agreement with 1.49 ± 0.07 for a much larger general sample with the amount of hidden close companions self-calibrated. I also investigate the radial profile of stacked sky-projected relative velocities without a deprojection to the 3D space. The observed profile matches the Newtonian predicted profile for s ≲ 2 kau without any free parameters, but shows a clear deviation at a larger separation with a significance of ≈5.0 σ . The projected velocity boost factor for s ≳ 5 kau is measured to be γ v p = 1.20 ± 0.06 (stat) ±0.05 (sys) matching γ g . Finally, for a small sample of 40 binaries with exceptionally precise radial velocities (fractional errors <0.005), the directly measured relative velocities in the 3D space also show a boost at larger separations. These results robustly confirm the recently reported gravitational anomaly at low acceleration for a general sample.