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Dark Matter (DM) and Modified Newtonian Dynamics (MOND) models ofrotationally supported galaxies lead to curves with different geometries in$(g_{N},g_{tot})$-space ($g2$-space). Here $g_{tot}$ is the total accelerationand $g_{N}$ is the acceleration as obtained from the baryonic matter viaNewtonian dynamics. In MOND modified inertia (MI) models the curves in$g2$-space are closed with zero area and so curve segments at radii $r\geqr_{N}$ (large radii) and $r< r_{N}$ (small radii) coincide, where $r_{N}$ isthe radius where $g_N$ is greatest. In DM models with cored density profileswhere $g_{tot}$ is also zero at the galactic centre, the curves are againclosed, but the area of the closed curves are in general non-zero because thecurve segments at radii $r\geq r_{N}$ and $r<r_{N}$ do not coincide. Finally inDM models with cuspy density profiles such as the NFW profile where $g_{tot}$is formally non-zero at the galactic origin the curves are open, and again thecurve segments at radii $r\geq r_{N}$ and $r< r_{N}$ do not coincide. Wedevelop a test of whether data at small and large radii coincide andinvestigate rotation curves from the SPARC database in order to discriminatebetween the above geometries. Due to loosely quantified systematicuncertainties we do not underline the result of the test, but instead concludethat the test illustrates the relevance of this type of analysis anddemonstrate the ability to discriminate between the considered DM and MI modelsin this way.

A Method for Discriminating Between Dark Matter Models and MOND Modified Inertia via Galactic Rotation Curves