Ultralight dark matter in disk galaxies

Abstract

Analytic arguments and numerical simulations show that bosonic ultralight dark matter (ULDM) would form cored density distributions ("solitons") at the center of galaxies. ULDM solitons offer a promising way to exclude or detect ULDM by looking for a distinctive feature in the central region of galactic rotation curves. Baryonic contributions to the gravitational potential pose an obstacle to such analyses, being (i) dynamically important in the inner galaxy and (ii) highly nonspherical in rotation-supported galaxies, resulting in nonspherical solitons. We present an algorithm for finding the ground-state soliton solution in the presence of stationary nonspherical background baryonic mass distribution. We quantify the impact of baryons on the predicted ULDM soliton in the Milky Way and in low-surface-brightness galaxies from the SPARC database.

Baryon-driven growth of solitonic cores in fuzzy dark matter halos

“…The density profile of the dark matter core with baryons is well described by a ground state solution of the SP equation taking into account the additional gravitational potential sourced by the baryon density. Similar solitonic solutions with an additional gravitating component have been investigated in the context of supermassive black holes [28,34] and galactic disks [33]. Our simulations confirm and extend these results by providing evidence that modified ground state solutions are approached dynamically in the presence of baryonic feedback (Appendix B).…”

Moments of nucleon generalized parton distributions from lattice QCD simulations at physical pion mass

“…4 and 5, respectively. The analysis of the cB211.072.64, for which we use seven values of t s with increased statistics, has clearly revealed that excited state effects die out slowly and that one needs to go to larger values of t s [35] keeping statistical errors small to see clear convergence as also demonstrated in Ref. [36].…”

“…3. (35) summation method at around t low s ≃1 fm converges to the two-state fit result within errors. We take the two-state fit result as our final value for these two ensembles.…”

“…(22) for the case of the two-point correlation function for the cB211.072.64 ensemble for the first 35 time-slices, i.e. t, t ′ ∈ [0,35]. From left to right, we showv tt ′ using n conf =30, 150, and 750 configurations.…”

Scalar field dark matter with a cosh potential, revisited

“…The results are not yet conclusive, and depending on the analysis one may argue for the presence of a soliton object and a SF mass of around m a22 ≡ (m a /10 −22 eV) 1, or just an upper bound for the latter, m a22 < 0.4. More recently, the very presence of a soliton structure has been tested using data from rotation curves in galaxies, and then it is inferred that m a22 > 10 [60,61].…”