Rotation curves of high-resolution LSB and SPARC galaxies with fuzzy and multistate (ultralight boson) scalar field dark matter

Abstract

Cold dark matter (CDM) has shown to be an excellent candidate for the dark matter (DM) of the Universe at large scales, however it presents some challenges at the galactic level. The scalar field dark matter (SFDM), also called fuzzy, wave, Bose-Einstein condensate or ultra-light axion DM, is identical to CDM at cosmological scales but different at the galactic ones. SFDM forms core halos, it has a natural cut-off in its matter power spectrum and it predicts well-formed galaxies at high redshifts. In this work we reproduce the rotation curves of high-resolution low surface brightness (LSB) and SPARC galaxies with two SFDM profiles: (1) The soliton+NFW profile in the fuzzy DM (FDM) model, arising empirically from cosmological simulations of real, non-interacting scalar field (SF) at zero temperature, and (2) the multistate SFDM (mSFDM) profile, an exact solution to the Einstein-Klein-Gordon equations for a real, self-interacting SF, with finite temperature into the SF potential, introducing several quantum states as a realistic model for a SFDM halo. From the fits with the soliton+NFW profile, we obtained for the boson mass 0.212 < m ψ /(10 −23 eV/c 2 ) < 27.0 and for the core radius 0.326 < r c /kpc < 8.96. From the combined analysis with the LSB galaxies, we obtained m ψ = 0.554 × 10 −23 eV, a result in tension with the severe cosmological constraints. Also, we show the analytical mSFDM model fits the observations as well as or better than the empirical soliton+NFW profile, and it reproduces naturally the wiggles present in some galaxies, being a theoretically motivated framework additional or alternative to the FDM profile.

Scalar field dark matter with a cosh potential, revisited

“…The presence of a central soliton in all of SFDM galaxy halos has motivated studies about galactic kinematics to infer, first, the presence of such soliton structure, and, second, to determine the mass scale of the underlying SF particle [38,[48][49][50][51][52][53][54][55][56][57][58][59][60][61][62][63]. 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.…”

Galaxy rotation curves using a non-parametric regression method: core, cuspy and fuzzy scalar field dark matter models

“…On the other hand, there is the so called cusp-core problem consisting in the observation that in some galaxies the center of the dark matter halo features a core behavior ρ D M ∼ constant, which is in disagreement with the cuspy behavior predicted by the simulations, ρ D M ∼ r −1 (for review see: de Blok (2010); Pontzen & Governato (2014)). Furthermore, by cosmological simulations Schive et al (2014), a density profile with inner solitonlike profile was derived, called Fuzzy, wave or ultra-light axion with an asymptotic NFW declination in the outer points, see Bernal et al (2018) and references therein for a review.…”

“…On the other hand, in the standard approach one selects a particular density profile or model of rotation curves, with a specific functional form between dependent and independent variables and then constrain the parameters of the chosen theory employing bayesian methods together observational data of galaxies (Bernal et al 2018;Garcia-Aspeitia et al 2017;Li et al 2019). The main problem of this method is the susceptibility to bias if the data is not well-represented by the assumed parametric model.…”

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

“…Less stringent constraints can be inferred from the high-z galaxy luminosity function [22][23][24][25][26]. Galaxies with measured rotation curves yield even lower masses than inferred from dwarf spheroidals [27] or at least exclude the typical value m ∼ 10 −22 eV [28,29]. In general, the scaling properties of solitons seem to disagree with observational data [30,31].…”