Observational Tests of Wave and Particle Dark Matter Predictions

Abstract

Recent discoveries of large halos of stars and dark matter around some of the lowest mass galaxies defy expectations that dwarf galaxies should be small and dense. Furthermore, these halos are seen to surround a dense core within each dwarf, with a clear density transition visible between the core and the halo at a radius of ' 1.0kpc. This common core-halo structure is hard to understand for standard heavy particle dark matter where featureless, concentrated profiles are predicted, whereas dark matter as a Bose-Einstein condensate, ψDM, naturally accounts for the observed profiles, predicting a dense soliton core in every galaxy surrounded by a tenuous halo of interfering waves. We show that the stellar profiles of the well studied "dwarf Spheroidal" (dSph) class, and also the equally numerous "ultra faint dwarfs" (UFD) are accurately fitted by the core-halo structure of ψDM, suggesting two boson species which are reinforced by parallel relations seen between the central density and radius of UDF and dSph dwarfs respectively, which both match the steep prediction, ρc ∝ R−^4c , for soliton cores in the ground state.

About the Speaker

Mr. Alvaro Pozo LARROCHA is a PhD student affiliated to both University of Basque Country and the Donostia International Physics Center, Donostia, Spain. His research interests include Wave Dark Matter and stellar behavior in galaxies under Wave Dark Matter conditions.

About the Program

For more information, please refer to the program website at http://iasprogram.ust.hk/particle_theory.