  The {\it Gaia} eDR3 catalogue has recently been used to study statistically
the internal kinematics of wide binary populations using relative velocities of
the two component stars, $\Delta V$, total binary masses, $m_{B}$, and
separations, $s$. For $s \gtrsim 0.01$ pc, these binaries probe the low
acceleration $a \lesssim 2a_{0}$ regime where gravitational anomalies usually
attributed to dark matter are observed in the flat rotation curves of spiral
galaxies, where $a_{0}\approx 1.2\times 10^{-10}$m s$^{-2}$ is the acceleration
scale of MOND. Such experiments test the degree of generality of these
anomalies, by exploring the same acceleration regime using independent
astronomical systems of vastly smaller mass and size. A signal above Newtonian
expectations has been observed when $a \lesssim 2a_{0}$, alternatively
interpreted as evidence of a modification of gravity, or as due to kinematic
contaminants; undetected stellar components, unbound encounters or spurious
projection effects. Here I take advantage of the enhanced DR3 {\it Gaia}
catalogue to perform a more rigorous study of the internal kinematics of wide
binaries than what has previously been possible. Internally determined {\it
Gaia} stellar masses and estimates of binary probabilities for each star using
spectroscopic information, together with a larger sample of radial velocities,
allow for a significant improvement in the analysis and careful exclusion of
possible kinematic contaminants. Resulting $\Delta V$ scalings accurately
tracing Newtonian expectations for the high acceleration regime, but markedly
inconsistent with these expectations in the low acceleration one, are obtained.
A non-Newtonian low acceleration phenomenology is thus confirmed.
