Distribution of Phantom Dark Matter in Dwarf Spheroidals
Alistair O. Hodson, Antonaldo Diaferio, and Luisa Ostorero

TL;DR
This paper models the distribution of phantom dark matter in dwarf spheroidal galaxies under MOND, considering their shape and external gravitational influences, predicting observable features that could test the theory.
Contribution
It provides a detailed prediction of phantom dark matter distribution in dwarf galaxies using axisymmetric models and external field effects within MOND, which can be tested observationally.
Findings
Offset of phantom dark matter in external field dominated dwarfs (~0.1-0.2 kpc)
Disturbed distribution with spikes where internal and external fields cancel
External field from large-scale structure has minor effect
Abstract
We derive the distribution of the phantom dark matter in the eight classical dwarf galaxies surrounding the Milky Way, under the assumption that modified Newtonian dynamics (MOND) is the correct theory of gravity. According to their observed shape, we model the dwarfs as axisymmetric systems, rather than spherical systems, as usually assumed. In addition, as required by the assumption of the MOND framework, we realistically include the external gravitational field of the Milky Way and of the large-scale structure beyond the Local Group. For the dwarfs where the external field dominates over the internal gravitational field, the phantom dark matter has, from the star distribution, an offset of ~0.1-0.2 kpc, depending on the mass-to-light ratio adopted. This offset is a substantial fraction of the dwarf half-mass radius. For Sculptor and Fornax, where the internal and external…
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