The diversity of core–halo structure in the fuzzy dark matter model

Chan, Hei Yin Jowett; Ferreira, Elisa G. M.; May, Simon; Hayashi, Kohei; Chiba, Masashi

doi:10.1093/mnras/stac063

Cited by 56 publications

(46 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…An investigation of whether VDM may naturally introduce more scatter (and change in observed slope) into its core shape and the core-halo mass relation, as our idealized simulations suggest they may, is needed. In more realistic simulations, there could be additional scatter due to tidal stripping as suggested by [33] for the SDM case. It is conceivable that ultralight VDM might ameliorate the existing tensions with observational data further.…”

Section: Dark Matter Cores In Dwarf Galaxiesmentioning

confidence: 94%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

View full text Add to dashboard Cite

We investigate the differences in the small-scale structure of vector dark matter (VDM) and scalar dark matter (SDM) using 3+1 dimensional simulations of single/multicomponent Schrödinger-Poisson system. We find that the amount of wave interference, core to halo mass ratio (and its scatter), spin of the core, as well as the shape of the central regions of dark matter halos can distinguish VDM and SDM. Starting with a collection of idealized halos (selfgravitating solitons) as an initial condition, we show that the system dynamically evolves to an approximately spherically symmetric configuration that has a core surrounded by a halo of interference patterns in the mass density. In the vector case, the central soliton in less dense and has a smoother transition to an r −3 tail compared to the scalar case. Wave interference is ∼ 1/ √ 3 times smaller in VDM compared to SDM, resulting in fewer low and high density regions in VDM compared to SDM, with more diffuse granules in the halo. The ratio of VDM core mass to the total halo mass is lower than that in SDM, with a steeper dependence on the total energy of the system and a slightly larger scatter. Finally, we also initiate a study of the evolution of intrinsic spin angular momentum in the VDM case. We see a positive correlation between the total intrinsic spin in the simulation and the spin of the final central core, with significant scatter. We see large intrinsic spin in the core being possible even with vanishing amounts total angular momentum in the initial conditions. Our results point towards the possibility of distinguishing VDM from SDM using astrophysical and terrestrial observations.

show abstract

Section: Dark Matter Cores In Dwarf Galaxiesmentioning

confidence: 94%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Different simulations yield different core-halo relations (e.g. Chan et al 2022;Schive et al 2014b;Mocz et al 2019;Mina et al 2020;Schwabe et al 2016;Nori & Baldi 2021;Yavetz et al 2022;Glennon et al 2022). For a summary of core-halo structures found in the literature, see Section 4.2.1 of Chan et al (2022).…”

Section: Uldm Halo Density Profilementioning

confidence: 99%

Quantum fluctuations masquerade as halos: Bounds on ultra-light dark matter from quadruply-imaged quasars

Alexander¹,

Gilman²,

Li³

et al. 2022

Preprint

View full text Add to dashboard Cite

Ultra-light dark matter (ULDM) refers to a class of theories, including ultra-light axions, in which particles with mass 𝑚 𝜓 < 10 −20 eV comprise a significant fraction of the dark matter. A galactic scale de Broglie wavelength distinguishes these theories from cold dark matter (CDM), suppressing the overall abundance of structure on sub-galactic scales, and producing wave-like interference phenomena in the density profiles of halos. With the aim of constraining the particle mass, we analyze the flux ratios in a sample of eleven quadruple-image strong gravitational lenses. We account for the suppression of the halo mass function and concentration-mass relation predicted by ULDM theories, and the wave-like fluctuations in the host halo density profile, calibrating the model for the wave interference against numerical simulations of galactic-scale halos. We show that the granular structure of halo density profiles, in particular, the amplitude of the fluctuations, significantly impacts image flux ratios, and therefore inferences on the particle mass derived from these data. We infer relative likelihoods of CDM to ULDM

show abstract

“…The diversity of ULP soliton density profiles is particularly interesting given the mild tension between the diversity of observed halos [71] and the predicted universal properties of Fuzzy dark matter solitons, see, e.g. [72][73][74] for a discussion and constraints. In the ULP model, a diversity of halos naturally emerges from adjusting the mixture of pions that make up the dark matter halo.…”

Section: Ulp Halos and Boson Starsmentioning

confidence: 99%

Ultra-Light Pion (ULP) and Baryon WIMPzilla Dark Matter

Maleknejad¹,

McDonough²

2022

Preprint

View full text Add to dashboard Cite

We consider a dark confining gauge theory with millicharged Ultra-Light Pions (ULP) and heavy baryons as dark matter candidates. The model simultaneously realizes the ultra-light (STronglyinteracting Ultralight Millicharged Particle or "STUMP") and superheavy ("WIMPzilla") dark matter paradigms, connected by the confinement scale of the dark QCD. It is a realization of millicharged ULDM, very unlike conventional axions, and exhibits a mass splitting between the charged and neutral pions. ULPs can easily provide the observed density of the dark matter, and be cosmologically stable, for a broad range of dark QCD scales and quark masses. The dark baryons, produced via gravitational particle production or via freeze-in, provide an additional contribution to the dark matter density. Dark matter halos and boson stars in this context are generically an admixture of the three pions and heavy baryons, leading to a diversity of density profiles. That opens up the accessible parameter space of the model compared with the standard millicharged DM scenarios and can be probed by future experiments. We briefly discuss additional interesting phenomenology, such as ULP electrodynamics, and Cosmic ULP Backgrounds. CONTENTS 8 4. Gravitational production 9 IV. ULP Halos and Boson Stars 9 V. Current Constraints and Avenues for Detection 11 VI. Discussion 12 A. Number density of heavy dark baryons 13 References 14

show abstract

The diversity of core–halo structure in the fuzzy dark matter model

Cited by 56 publications

References 35 publications

Small-scale structure in vector dark matter

Small-scale structure in vector dark matter

Quantum fluctuations masquerade as halos: Bounds on ultra-light dark matter from quadruply-imaged quasars

Ultra-Light Pion (ULP) and Baryon WIMPzilla Dark Matter

Contact Info

Product

Resources

About