Galactic rotation curves versus ultralight dark matter: A systematic comparison with SPARC data

Abstract

We look for and place observational constraints on the imprint of ultralight dark matter (ULDM) soliton cores in rotation-dominated galaxies. Extending previous analyses, we find a conservative, modelindependent constraint which disfavours the soliton-host halo relation found in numerical simulations over a broad range in the ULDM particle mass m. Combining the observational constraints with theoretical arguments for the efficiency of soliton formation via gravitational dynamical relaxation, our results disfavour ULDM from comprising 100% of the total cosmological dark matter in the range 10 −24 eV m 10 −20 eV. The constraints probe the ULDM fraction down to f 0.3 of the total dark matter.

Not so fuzzy: excluding FDM with sizes and stellar kinematics of ultra-faint dwarf galaxies

“…Early work using FDM simulations found a tight scaling relation between the soliton mass and the virial mass of the host halo [8], leading to a number of papers attempting to constrain the FDM particle mass by finding evidence for either the presence or absence of massive solitons in nearby galaxies [9][10][11][12][13]. More recent FDM simulations covering larger cosmological volumes, however, discount the existence of a tight scaling relation between * ndalal@pitp.ca soliton mass and host halo mass, and instead indicate a large scatter in the correlation [14,15].…”

Closing the window on fuzzy dark matter with the 21cm signal

“…In pink, bounds from galaxy weak lensing combined with Planck (+DES) [40]. In purple, bounds from galaxy rotation curves (SPARC) [41]. In grey, bounds from the M87 black hole spin, derived from the non-observation of superradiance [42][43][44].…”