We explore the possibility that the dark matter (DM) component in galaxies may originate fractional gravity. In
such a framework, the standard law of inertia continues to hold, but the gravitational potential associated with a
given DM density distribution is determined by a modified Poisson equation including fractional derivatives (i.e.,
derivatives of noninteger type) that are meant to describe nonlocal effects. We analytically derive the expression of
the potential that in fractional gravity corresponds to various spherically symmetric density profiles, including the
Navarro–Frenk–White (NFW) distribution that is usually exploited to describe virialized halos of collisionless DM
as extracted from N-body cosmological simulations. We show that in fractional gravity, the dynamics of a test
particle moving in a cuspy NFW density distribution is substantially altered with respect to the Newtonian case,
mirroring what in Newtonian gravity would instead be sourced by a density profile with an inner core. We test the
fractional gravity framework on galactic scales, showing that (i) it can provide accurate fits to the stacked rotation
curves of spiral galaxies with different properties, including dwarfs; (ii) it can reproduce to reasonable accuracy the
observed shape and scatter of the radial acceleration relation over an extended range of galaxy accelerations; and
(iii) it can properly account for the universal surface density and the core radius versus disk scale length scaling
relations. Finally, we discuss the possible origin of the fractional gravity behavior as a fundamental or emerging
property of the elusive DM component.
