Warm dark matter

Short description: Hypothesized form of dark matter

Warm dark matter (WDM) is a hypothesized form of dark matter that has properties intermediate between those of hot dark matter and cold dark matter, causing structure formation to occur bottom-up from above their free-streaming scale, and top-down below their free streaming scale. The most common WDM candidates are sterile neutrinos and gravitinos. The WIMPs (weakly interacting massive particles), when produced non-thermally, could be candidates for warm dark matter. In general, however, the thermally produced WIMPs are cold dark matter candidates.

## Contents

* 1 keVins and GeVins
* 2 See also
* 3 References
* 4 Further reading

## keVins and GeVins

One possible WDM candidate particle with a mass of a few keV comes from introducing two new, zero charge, zero lepton number fermions to the Standard Model of Particle Physics: "keV-mass inert fermions" (keVins) and "GeV-mass inert fermions" (GeVins). keVins are overproduced if they reach thermal equilibrium in the early universe, but in some scenarios the entropy production from the decays of unstable heavier particles may suppress their abundance to the correct value. These particles are considered "inert" because they only have suppressed interactions with the Z boson.

Sterile neutrinos with masses of a few keV are possible candidates for keVins.

At temperatures below the electroweak scale their only interactions with standard model particles are weak interactions due to their mixing with ordinary neutrinos. Due to the smallness of the mixing angle they are not overproduced because they freeze out before reaching thermal equilibrium. Their properties are consistent with astrophysical bounds coming from structure formation and the Pauli principle if their mass is larger than 1-8 keV.

In February 2014, different analyses[1][2] have extracted from the spectrum of X-ray emissions observed by XMM-Newton, a monochromatic signal around 3.5 keV. This signal is coming from different galaxy clusters (like Perseus and Centaurus) and several scenarios of warm dark matter can justify such a line. We can cite, for example, a 3.5 keV candidate annihilating into 2 photons,[3] or a 7 keV dark matter particle decaying into a photon and a neutrino.[4]

In November 2019, analysis of the interaction of various galactic halo matter on densities and distribution of stellar streams, coming off the satellites of the Milky Way, they were able to constrain minimums of mass for density perturbations by warm dark matter keVins in the GD-1 and Pal 5 streams. This lower limit on the mass of warm dark matter thermal relics mWDM > 4.6 keV; or adding dwarf satellite counts mWDM > 6.3 keV.[5]

## See also

* Astronomy:Dark matter - Hypothetical invisible cosmic material
* Astronomy:Hot dark matter (HDM) - Theoretical form of dark matter particles which travel near the speed of light
* Astronomy:Cold dark matter (CDM) - Hypothetical type of dark matter in physics
* Astronomy:Lambda-CDM model - Mathematical model of the Big Bang
* Astronomy:Modified Newtonian dynamics - Hypothesis proposing a modification of Newton's laws

## References

1. ↑ Bulbul, Esra; Markevitch, Maxim; Foster, Adam; Smith, Randall K.; Loewenstein, Michael; Randall, Scott W. (2014-06-10). "Detection of an Unidentified Emission Line in the Stacked X-Ray Spectrum of Galaxy Clusters". The Astrophysical Journal 789 (1): 13. doi:10.1088/0004-637x/789/1/13. ISSN 0004-637X. Bibcode: 2014ApJ...789...13B.
2. ↑ Boyarsky, A.; Ruchayskiy, O.; Iakubovskyi, D.; Franse, J. (2014-12-15). "Unidentified Line in X-Ray Spectra of the Andromeda Galaxy and Perseus Galaxy Cluster". Physical Review Letters 113 (25). doi:10.1103/physrevlett.113.251301. ISSN 0031-9007. PMID 25554871. Bibcode: 2014PhRvL.113y1301B.
3. ↑ Dudas, Emilian; Heurtier, Lucien; Mambrini, Yann (2014-08-04). "Generating x-ray lines from annihilating dark matter". Physical Review D 90 (3). doi:10.1103/physrevd.90.035002. ISSN 1550-7998. Bibcode: 2014PhRvD..90c5002D.
4. ↑ Ishida, Hiroyuki; Jeong, Kwang Sik; Takahashi, Fuminobu (2014). "7 keV sterile neutrino dark matter from split flavor mechanism". Physics Letters B 732: 196–200. doi:10.1016/j.physletb.2014.03.044. ISSN 0370-2693. Bibcode: 2014PhLB..732..196I.
5. ↑ Banik, Nilianjan; Bovy, Jo; Bertone, Gianfranco; Erkal, Denis; de Boer, T.J.L (2021). "Novel constraints on the particle nature of dark matter from stellar streams". Journal of Cosmology and Astroparticle Physics 2021 (10): 043. doi:10.1088/1475-7516/2021/10/043. Bibcode: 2021JCAP...10..043B.

* Viel, Matteo; Lesgourgues, Julien; Haehnelt, Martin G.; Matarrese, Sabino; Riotto, Antonio (2005-03-31). "Constraining warm dark matter candidates including sterile neutrinos and light gravitinos with WMAP and the Lyman-αforest". Physical Review D 71 (6): 063434. doi:10.1103/physrevd.71.063534. ISSN 1550-7998. Bibcode: 2005PhRvD..71f3534V.
* King, Stephen F; Merle, Alexander (2012-08-16). "Warm Dark Matter from keVins". Journal of Cosmology and Astroparticle Physics 2012 (8): 016. doi:10.1088/1475-7516/2012/08/016. ISSN 1475-7516. Bibcode: 2012JCAP...08..016K.
* Gao, L.; Theuns, T. (2007-09-14). "Lighting the Universe with Filaments". Science 317 (5844): 1527–1530. doi:10.1126/science.1146676. ISSN 0036-8075. PMID 17872439. Bibcode: 2007Sci...317.1527G.
* Lin, W. B.; Huang, D. H.; Zhang, X.; Brandenberger, R. (2001-02-05). "Nonthermal Production of Weakly Interacting Massive Particles and the Subgalactic Structure of the Universe". Physical Review Letters 86 (6): 954–957. doi:10.1103/physrevlett.86.954. ISSN 0031-9007. PMID 11177983. Bibcode: 2001PhRvL..86..954L.
* Millis, John. Warm Dark Matter. About.com. Retrieved 23 Jan., 2013. http://space.about.com/od/astronomydictionary/g/Warm-Dark-Matter.htm .

## Further reading

* Bertone, Gianfranco (2010). Particle Dark Matter: Observations, Models and Searches. Cambridge University Press. p. 762. ISBN 978-0-521-76368-4.

* v
* t
* e

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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