Abstract
This paper studies a model of dark matter called wave dark matter (also known as scalar field dark matter and boson stars). Wave dark matter describes dark matter as a scalar field which satisfies the Einstein-Klein-Gordon equations. These equations rely on a fundamental constant ϒ (also known as the “mass term” of the Klein-Gordon equation), which can be interpreted physically as a characteristic frequency of the scalar field. In this work, we compare the wave dark matter model to observations to obtain an estimate of ϒ. Specifically, we compare the mass profiles of spherically symmetric static states of wave dark matter to certain Burkertmass profiles recently shown to predict well the velocity dispersion profiles of the eight classical dwarf spheroidal galaxies. We outline a procedure for estimating ϒ in these circumstances and show that under precise assumptions the value of ϒ can be bounded above by 1000 yr−1. We also show that a reasonable working value for this constant is ϒ = 50 yr−1.
Highlights
Ever since the first postulation of dark matter in the 1930’s by Zwicky [40], much evidence for the existence of dark matter has accumulated including the unexpected behavior in the rotation curves of spiral galaxies [2,8], the velocity dispersion profiles of dwarf spheroidal galaxies [31, 37,38,39], and gravitational lensing [13]
The Navarro-Frenk-White dark matter energy density profile exhibits an infinite cusp at the origin, while observations favor a bounded value of the dark matter energy density at the centers of galaxies [14, 15]
Our goal is to find a value of Υ that is compatible with the Burkert mass profiles that Salucci et al [31] computed to model the dark matter in the eight classical dwarf spheroidal galaxies
Summary
Ever since the first postulation of dark matter in the 1930’s by Zwicky [40], much evidence for the existence of dark matter has accumulated including the unexpected behavior in the rotation curves of spiral galaxies [2,8], the velocity dispersion profiles of dwarf spheroidal galaxies [31, 37,38,39], and gravitational lensing [13] These and other observations support the idea that most of the matter in the universe is not baryonic, but is, some form of exotic dark matter and that almost all astronomical objects from the galactic scale and up contain a significant amount of this dark matter.
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