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arXiv · 2512.15886

Cored galaxies in cuspy dark matter halos

Fernando Valenciano·Jorge Martin Camalich·Arianna Di Cintio·Julio F. Navarro·Giuseppina Battaglia·Raphaël Errani·Justin I. Read
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Abstract

We investigate constraints on the inner stellar density profile from photometric data of dwarf spheroidal and ultra-faint dwarf galaxies. Our aim is to clarify under what conditions cored stellar profiles require dark matter halos that are also cored, deviating from the cuspy profiles expected for cold dark matter halos. We consider a variety of spherically symmetric stellar profiles, which we classify as "strong" or "weak" cores and cusps according to the behavior of the slope ($b_0$) and logarithmic slope ($\gamma_0$) at their centers. We explore which profiles lead to unphysical negative distribution functions when embedded in a cuspy halo, treating isotropic and anisotropic kinematics separately. We find that weakly-cored stellar profiles in 3D (i.e., $b_0 \neq 0$, $\gamma_0=0$) can be consistent with cuspy dark matter profiles, but strong 3D cores ($b_0=\gamma_0=0$) are not. However, both weak and strong 3D cores yield nearly indistinguishable inner profiles in projection, which implies that ruling out a dark matter cusp from photometric data alone is highly challenging. As an example, we study the profiles of ultra-faint dwarf galaxies and find that they are consistent with both weak and strong 3D cores. This is not just a result of the limited numbers of stars in these systems, since we reach the same conclusion even for Fornax, one of the most luminous and best-studied dwarf spheroidal companions of the Milky Way. We conclude that, based on current data and analysis techniques, cored surface density profiles in nearby dwarf galaxies cannot be taken as strong evidence against the presence of cuspy dark matter halos.

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Fernando Valenciano, Jorge Martin Camalich, Arianna Di Cintio, Julio F. Navarro, Giuseppina Battaglia, Raphaël Errani, Justin I. Read. 2025-12-17. Cored galaxies in cuspy dark matter halos. https://doi.org/10.1051/0004-6361%2F202558629

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