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Galactic rotation curves versus ultralight dark matter: A systematic comparison with SPARC data
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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 constraint which disfavors the soliton-host halo relation found in some 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, and assuming that the soliton-halo relation is correct, our results disfavor ULDM from comprising 100\% of the total cosmological dark matter in the range $10^{-24}~{\rm eV}\lesssim m\lesssim10^{-20}~{\rm eV}$. The constraints probe the ULDM fraction down to $f\lesssim0.3$ of the total dark matter.
Forward citations
Cited by 2 Pith papers
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Learning from galactic rotation curves: a neural network approach
Neural networks trained on simulated rotation curves can infer ultra-light dark matter and baryonic parameters from SPARC dwarf galaxies, with uncertainties comparable to MCMC.
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Self-interactions of ultralight spinless dark matter to the rescue?
A quartic self-coupling around 10^-90 can allow 10^-22 eV scalar dark matter to match galaxy rotation curves and the soliton-halo relation, softening bounds derived for non-interacting ULDM.
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