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Galactic rotation curves are often considered the first robust evidence forthe existence of dark matter. However, even in the presence of a dark matterhalo, other galactic-scale observations, such as the Baryonic Tully-FisherRelation and the Radial Acceleration Relation, remain challenging to explain.This has motivated long-distance, infrared modifications to gravity as analternative to the dark matter hypothesis as well as various DM theories withsimilar phenomenology. In general, the standard lore has been that any modelthat reduces to the phenomenology of MOdified Newtonian Dynamics (MOND) ongalactic scales explains essentially all galaxy-scale observables. We present aframework to test precisely this statement using local Milky Way observables,including the vertical acceleration field, the rotation curve, the baryonicsurface density, and the stellar disk profile. We focus on models that predictscalar amplifications of gravity, i.e., models that increase the magnitude butdo not change the direction of the gravitational acceleration. We find thatmodels of this type are disfavored relative to a simple dark matter halo modelbecause the Milky Way data requires a substantial amplification of the radialacceleration with little amplification of the vertical acceleration. Weconclude that models which result in a MOND-like force struggle tosimultaneously explain both the rotational velocity and vertical motion ofnearby stars in the Milky Way.

Testing Dark Matter and Modifications to Gravity using Local Milky Way Observables