Plan beta: Core or Cusp?

Abstract

The inner profile of Dark Matter (DM) halos remains one of the central problems in small-scale cosmology. At present, the problem can not be resolved in dwarf spheroidal galaxies due to a degeneracy between the DM profile and the velocity anisotropy beta of the stellar population. We discuss a method which can break the degeneracy by exploiting 3D positions and 1D line-of-sight (LOS) velocities. With the full 3D spatial information, we can determine precisely what fraction of each stars LOS motion is in the radial and tangential direction. This enables us to infer the anisotropy parameter beta directly from the data. The method is particularly effective if the galaxy is highly anisotropic. Finally, we argue that such a test could be applied to Sagittarius and potentially other dwarfs with RR Lyrae providing the necessary depth information.

10 pages, 3 figures Accepted in MNRAS. Extended introduction to match accepted version. Main conclusions unchanged

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• A critical reassessment of particle Dark Matter limits from dwarf satellites
• The Cusp/Core problem: supernovae feedback versus the baryonic clumps and dynamical friction model
• Three-dimensional structure of the Sagittarius dSph core from RR Lyrae
• On the dark matter haloes inner structure and galaxy morphology
• The proper motion of stars in dwarf galaxies: distinguishing central density cusps from cores
• What can Gaia (with TMT) say about Sculptor's Core?
• Kinematics of the Sagittarius Dwarf Spheroidal core: A 5D Analysis for a 6D Methodology with Gaia DR3