Fuzzy cold dark matter

Short description: Hypothetical form of cold dark matter proposed to solve the cuspy halo problem

Fuzzy cold dark matter is a hypothetical form of cold dark matter proposed to solve the cuspy halo problem. It would consist of extremely light scalar particles with masses on the order of ≈10−22 eV; so a Compton wavelength on the order of 1 light year. Fuzzy cold dark matter halos in dwarf galaxies would manifest wave behavior on astrophysical scales, and the cusps would be avoided through the Heisenberg uncertainty principle.[1] The wave behavior leads to interference patterns, spherical soliton cores in dark matter halo centers,[2] and cylindrical soliton-like cores in dark matter cosmic web filaments.[3]

Fuzzy cold dark matter is a limit of scalar field dark matter without self-interaction.[4][5] Fuzzy cold dark matter is sometimes called wave DM, or simply fuzzy dark matter (FDM).[6] It is governed by the Schrödinger–Poisson equation.

Fuzzy dark matter models are the simplest class of the ultralight dark matter models; the only free parameter is the particle mass. (In "ultralight dark matter models", the dark matter of a galaxy condenses into a superfluid. This requirement greatly constrains the particle mass; for example, the QCD (Peccei–Quinn) axion is considered too heavy to condense.) A second approach, where FDM is modified to have simple self-interaction, has been suggested with theories such as self-interacting fuzzy dark matter (SIFDM), repulsive DM, scalar field DM, and fluid dark matter. A third approach, called the "DM superfluid model", focuses on the empirical data for a large-scale MOND relation, and then works backwards to determine what types of complicated self-interactions would best produce such a distribution.[6]

New research (2023) has uncovered evidence that fuzzy dark matter, specifically ultralight axions, may better fit gravitational lens data than WIMP dark matter.[7]

## Notes

1. ↑ Hu, Wayne; Barkana, Rennan; Gruzinov, Andrei (2000). "Cold and Fuzzy Dark Matter". Physical Review Letters 85 (6): 1158–61. doi:10.1103/PhysRevLett.85.1158. PMID 10991501. Bibcode: 2000PhRvL..85.1158H.
2. ↑ Schive, Hsi-Yu; Chiueh, Tzihong; Broadhurst, Tom (2014). "Cosmic structure as the quantum interference of a coherent dark wave". Nature Physics 10 (7): 496–499. doi:10.1038/nphys2996. Bibcode: 2014NatPh..10..496S.
3. ↑ Mocz, Philip; Fialkov, Anastasia; Vogelsberger, Mark; Becerra, Fernando; Amin, Mustafa A.; Bose, Sownak; Boylan-Kolchin, Michael; Chavanis, Pierre-Henri et al. (2019). "First Star-Forming Structures in Fuzzy Cosmic Filaments". Physical Review Letters 123 (14). doi:10.1103/PhysRevLett.123.141301. ISSN 0031-9007. PMID 31702225. Bibcode: 2019PhRvL.123n1301M.
4. ↑ Bohua Li; Tanja Rindler-Daller; Paul R. Shapiro (2014). "Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter". Phys. Rev. D 89 (8). doi:10.1103/PhysRevD.89.083536. Bibcode: 2014PhRvD..89h3536L.
5. ↑ Lee, Jae-Weon (2018). "Brief History of Ultra-light Scalar Dark Matter Models". EPJ Web of Conferences 168: 06005. doi:10.1051/epjconf/201816806005. Bibcode: 2018EPJWC.16806005L.
6. ↑ 6.0 6.1 Ferreira, Elisa G. M. (December 2021). "Ultra-light dark matter". The Astronomy and Astrophysics Review 29 (1): 7. doi:10.1007/s00159-021-00135-6. Bibcode: 2021A&ARv..29....7F.
7. ↑ Timmer, John (2023-04-21). "No WIMPS! Heavy particles don't explain gravitational lensing oddities". https://arstechnica.com/science/2023/04/gravitational-lensing-may-point-to-lighter-dark-matter-candidate/.

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Dark matter

Forms of dark matter|

* Baryonic dark matter
* Cold dark matter
* Hot dark matter
* Light dark matter
* Mixed dark matter
* Warm dark matter
* Self-interacting dark matter
* Scalar field dark matter
* Primordial black holes

Hypothetical particles|

* Axino
* Axion
* Dark photon
* Holeum
* LSP
* Minicharged particle
* Neutralino
* Sterile neutrino
* SIMP
* WIMP

Theories and objects|

* Cuspy halo problem
* Dark fluid
* Dark galaxy
* Dark globular cluster
* Dark matter halo
* Dark radiation
* Dark star
* Dwarf galaxy problem
* Halo mass function
* Mass dimension one fermions
* Massive compact halo object
* Mirror matter
* Navarro–Frenk–White profile
* Scalar field dark matter

Search experiments|

| Direct detection|

* ADMX
* ANAIS
* ArDM
* CDEX
* CDMS
* CLEAN
* CoGeNT
* COSINE
* COUPP
* CRESST
* CUORE
* D3
* DAMA/LIBRA
* DAMA/NaI
* DAMIC
* DarkSide
* DARWIN
* DEAP
* DM-Ice
* DMTPC
* DRIFT
* EDELWEISS
* EURECA
* KIMS
* LUX
* LZ
* MACRO
* MIMAC
* NAIAD
* NEWAGE
* NEWS-G
* PandaX
* PICASSO
* PICO
* ROSEBUD
* SABRE
* SIMPLE
* TREX-DM
* UKDMC
* WARP
* XENON
* XMASS
* ZEPLIN

|

Indirect detection|

* AMS-02
* ANTARES
* ATIC
* CALET
* CAST
* DAMPE
* Fermi
* HAWC
* HESS
* IceCube
* MAGIC
* MOA
* OGLE
* PAMELA
* VERITAS

Other projects|

* MultiDark
* PVLAS

Potential dark galaxies|

* HE0450-2958
* HVC 127-41-330
* Smith's Cloud
* VIRGOHI21

Related|

* Antimatter
* Dark energy
* Exotic matter
* Galaxy formation and evolution
* Illustris project
* Imaginary mass
* Negative mass
* UniverseMachine

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