Galactic kinematics with modified Newtonian dynamics
O. Bienaym\'e, B. Famaey, X. Wu, H.S. Zhao, D. Aubert

TL;DR
This paper investigates observational methods to distinguish between Newtonian gravity and MOND in the Milky Way by analyzing disk surface density, mass gradients, and velocity ellipsoid tilt, especially with upcoming large surveys like GAIA.
Contribution
It proposes specific observational signatures that can differentiate MOND from Newtonian models in the Milky Way using current and future data.
Findings
Predicted local surface density of ~78 Msun/pc2 if MOND applies.
Expected increase in disk scale-length by a factor of 1.25 under MOND.
Vertical tilt of velocity ellipsoid at 6 degrees above the plane.
Abstract
We look for observational signatures that could discriminate between Newtonian and modified Newtonian (MOND) dynamics in the Milky Way, in view of the advent of large astrometric and spectroscopic surveys. Indeed, a typical signature of MOND is an apparent disk of "phantom" dark matter, which is uniquely correlated with the visible disk-density distribution. Due to this phantom dark disk, Newtonian models with a spherical halo have different signatures from MOND models close to the Galactic plane. The models can thus be differentiated by measuring dynamically (within Newtonian dynamics) the disk surface density at the solar radius, the radial mass gradient within the disk, or the velocity ellipsoid tilt angle above the Galactic plane. Using the most realistic possible baryonic mass model for the Milky Way, we predict that, if MOND applies, the local surface density measured by a…
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