Kavli Affiliate: Andrey Kravtsov
| First 5 Authors: Simon May, Simon May, , ,
| Summary:
The particle mass of dark matter (DM) was previously constrained using
kinematics of ultra-faint dwarf galaxies to $m > 3 times
10^-19,mathrmeV$. This constraint, which excludes the "fuzzy" range of
ultra-light dark matter from comprising all of the DM, relies on an estimate of
the heating rate from fuzzy dark matter (FDM) wave interference using linear
perturbation theory. Here, we compare the results of this perturbative
calculation to full Schr"odinger-Poisson simulations of the evolution of star
particles in FDM halos. This comparison confirms theoretical expectations that
FDM heating is stronger in fully nonlinear simulations due to the formation of
a dense central soliton whose fluctuations enhance gravitational perturbations,
and that bounds on the DM particle mass using this perturbative method are
indeed conservative. We also show that these bounds are not affected by
possible tidal stripping, since for dwarf satellites like Segue 1, the tidal
radius is much larger than the observed size of the galaxy. We further show
that the constraints on the mass cannot be evaded by invoking DM
self-interactions, due to constraints on the self-interaction from large-scale
structure. Lastly, we show that if the recently discovered system Ursa Major
III/UNIONS I is a galaxy, the observed properties of this object strengthen the
lower bound on the DM mass by over an order of magnitude, to $m > 8 times
10^-18,mathrmeV$, at 95% confidence. This constraint could further be
strengthened considerably by more precise measurements of the size and velocity
dispersion of this and other similar galaxies, and by using full
Schr"odinger-Poisson simulations.
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