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{{short description|Hypothetical particles that
{{redirect|WIMPs||WIMPS (disambiguation)}}
'''Weakly interacting massive particles''' ('''WIMPs''') are hypothetical particles that are one of the proposed candidates for [[dark matter]].
There exists no formal definition of a WIMP, but broadly,
Experimental efforts to detect WIMPs include the search for products of WIMP annihilation, including [[gamma ray]]s, [[neutrino]]s and [[cosmic ray]]s in nearby galaxies and galaxy clusters; direct detection experiments designed to measure the collision of WIMPs with [[Atomic nucleus|nuclei]] in the laboratory, as well as attempts to directly produce WIMPs in colliders, such as the
Because [[supersymmetry|supersymmetric]] extensions of the
== Theoretical framework and properties ==
WIMP-like particles are predicted by [[R-parity]]-conserving [[supersymmetry]], a
▲WIMP-like particles are predicted by [[R-parity]]-conserving [[supersymmetry]], a popular type of extension to the [[Standard Model]] of particle physics, although none of the large number of new particles in supersymmetry have been observed.<ref>{{cite book |last1=Klapdor-Kleingrothaus |first1=H.V. |year=1998 |chapter=Double beta decay and dark matter search - window to new physics now, and in future (GENIUS) |title=Beyond the Desert |editor1=Klapdor-Kleingrothaus, V. |editor2=Paes, H. |publisher=IOP |volume=1997 |page=485 |bibcode = 1998hep.ex....2007K |arxiv=hep-ex/9802007}}</ref>
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The main theoretical characteristics of a WIMP are:
* Interactions only through the [[weak nuclear force]] and [[gravity]], or possibly other interactions with [[Cross section (physics)|cross-sections]] no higher than the weak scale;<ref name="Kamionkowski">{{cite journal |arxiv=hep-ph/9710467 |last1=Kamionkowski |first1=Marc |title=WIMP and Axion Dark Matter |journal=High Energy Physics and Cosmology |volume=14 |pages=394 |year=1997|bibcode=1998hepc.conf..394K }}</ref>
* Large mass compared to standard particles (WIMPs with sub-[[Electron volt|GeV]]/''c''<sup>2</sup> masses may be considered to be [[light dark matter]]).
Because of their lack of electromagnetic interaction with normal matter, WIMPs would be invisible through normal electromagnetic observations. Because of their large mass, they would be relatively slow moving and therefore "cold".<ref>{{cite
== As dark matter ==
A decade after the dark matter problem was established in the 1970s, WIMPs were suggested as a potential solution to the issue.<ref>{{cite journal|last1=de Swart|first1=J. G.|last2=Bertone|first2=G.|last3=van Dongen|first3=J.|title=How dark matter came to matter|journal=Nature Astronomy|date=2017|volume=1|issue=59|pages=0059|doi=10.1038/s41550-017-0059|arxiv = 1703.00013 |bibcode = 2017NatAs...1E..59D |s2cid=119092226}}</ref> Although the existence of WIMPs in nature is still hypothetical, it would resolve a number of astrophysical and cosmological problems related to dark matter. There is consensus today among astronomers that most of the mass in the Universe is indeed dark. Simulations of a universe full of cold dark matter produce galaxy distributions that are roughly similar to what is observed.<ref>{{
WIMPs fit the model of a relic dark matter particle from the early Universe, when all particles were in a state of [[thermal equilibrium]]. For sufficiently high temperatures, such as those existing in the early Universe, the dark matter particle and its antiparticle would have been both forming from and annihilating into lighter particles. As the Universe expanded and cooled, the average thermal energy of these lighter particles decreased and eventually became insufficient to form a dark matter particle-antiparticle pair. The annihilation of the dark matter particle-antiparticle pairs, however, would have continued, and the number density of dark matter particles would have begun to decrease exponentially.<ref name="Kamionkowski" /> Eventually, however, the number density would become so low that the dark matter particle and antiparticle interaction would cease, and the number of dark matter particles would remain (roughly) constant as the Universe continued to expand.<ref name="Griest" /> Particles with a larger interaction cross section would continue to annihilate for a longer period of time, and thus would have a smaller number density when the annihilation interaction ceases. Based on the current estimated abundance of dark matter in the Universe, if the dark matter particle is such a relic particle, the interaction cross section governing the particle-antiparticle annihilation can be no larger than the cross section for the weak interaction.<ref name="Kamionkowski" /> If this model is correct, the dark matter particle would have the properties of the WIMP.
== Indirect detection ==
{{see also|Indirect detection of dark matter}}
Because WIMPs may only interact through gravitational and weak forces, they would be extremely difficult to detect. However, there are many experiments underway to attempt to detect WIMPs both directly and indirectly. ''Indirect detection'' refers to the observation of annihilation or decay products of WIMPs far away from Earth. Indirect detection efforts typically focus on locations where WIMP dark matter is thought to accumulate the most: in the centers of galaxies and galaxy clusters, as well as in the smaller [[Satellite galaxy|satellite galaxies]] of the Milky Way. These are particularly useful since they tend to contain very little baryonic matter, reducing the expected background from standard astrophysical processes. Typical indirect searches look for excess [[gamma rays]], which are predicted both as final-state products of annihilation, or are produced as charged particles interact with ambient radiation via [[inverse Compton scattering]]. The spectrum and intensity of a gamma ray signal depends on the annihilation products, and must be computed on a model-by-model basis. Experiments that have placed bounds on WIMP annihilation, via the non-observation of an annihilation signal, include the [[Fermi Gamma-ray Space Telescope|Fermi]]-LAT gamma ray telescope<ref>{{cite journal |doi=10.1103/PhysRevD.89.042001 |title=Dark matter constraints from observations of 25 Milky Way satellite galaxies with the Fermi Large Area Telescope |date=2014 |collaboration=The Fermi-LAT Collaboration |journal=Physical Review D |volume=89 |issue=4 |pages=042001 |arxiv=1310.0828 |last1=Ackermann |first1=M. |display-authors=etal |bibcode=2014PhRvD..89d2001A |s2cid=46664722 }}</ref> and the VERITAS ground-based gamma ray observatory.<ref>{{cite journal |last1=Grube |first1=Jeffrey |title=VERITAS Limits on Dark Matter Annihilation from Dwarf Galaxies |pages=689–692 |author2=VERITAS Collaboration |year=2012 |doi=10.1063/1.4772353 |journal=AIP Conference Proceedings|volume=1505 |bibcode=2012AIPC.1505..689G |arxiv = 1210.4961 |s2cid=118510709 }}</ref> Although the annihilation of WIMPs into Standard Model particles also predicts the production of high-energy neutrinos, their interaction rate is thought to be too low to reliably detect a dark matter signal at present. Future observations from the [[IceCube]] observatory in Antarctica may be able to differentiate WIMP-produced neutrinos from standard astrophysical neutrinos; however, by 2014, only 37 cosmological neutrinos had been observed,<ref>{{cite journal |doi=10.1103/PhysRevLett.113.101101 |pmid=25238345 |title=Observation of High-Energy Astrophysical Neutrinos in Three Years of IceCube Data |date=2014 |collaboration=IceCube Collaboration▼
▲Indirect detection efforts typically focus on locations where WIMP dark matter is thought to accumulate the most: in the centers of galaxies and galaxy clusters, as well as in the smaller [[Satellite galaxy|satellite galaxies]] of the Milky Way. These are particularly useful since they tend to contain very little baryonic matter, reducing the expected background from standard astrophysical processes. Typical indirect searches look for excess [[gamma rays]], which are predicted both as final-state products of annihilation, or are produced as charged particles interact with ambient radiation via [[inverse Compton scattering]]. The spectrum and intensity of a gamma ray signal depends on the annihilation products, and must be computed on a model-by-model basis. Experiments that have placed bounds on WIMP annihilation, via the non-observation of an annihilation signal, include the [[Fermi Gamma-ray Space Telescope|Fermi]]-LAT gamma ray telescope<ref>{{cite journal |doi=10.1103/PhysRevD.89.042001 |title=Dark matter constraints from observations of 25 Milky Way satellite galaxies with the Fermi Large Area Telescope |date=2014 |collaboration=The Fermi-LAT Collaboration |journal=Physical Review D |volume=89 |issue=4 |pages=042001 |arxiv=1310.0828 |last1=Ackermann |first1=M. |display-authors=etal |bibcode=2014PhRvD..89d2001A |s2cid=46664722 }}</ref> and the VERITAS ground-based gamma ray observatory.<ref>{{cite journal |last1=Grube |first1=Jeffrey |title=VERITAS Limits on Dark Matter Annihilation from Dwarf Galaxies |pages=689–692 |author2=VERITAS Collaboration |year=2012 |doi=10.1063/1.4772353 |journal=AIP Conference Proceedings|volume=1505 |bibcode=2012AIPC.1505..689G |arxiv = 1210.4961 |s2cid=118510709 }}</ref> Although the annihilation of WIMPs into Standard Model particles also predicts the production of high-energy neutrinos, their interaction rate is too low to reliably detect a dark matter signal at present. Future observations from the [[IceCube]] observatory in Antarctica may be able to differentiate WIMP-produced neutrinos from standard astrophysical neutrinos; however, by 2014, only 37 cosmological neutrinos had been observed,<ref>{{cite journal |doi=10.1103/PhysRevLett.113.101101 |pmid=25238345 |title=Observation of High-Energy Astrophysical Neutrinos in Three Years of IceCube Data |date=2014 |collaboration=IceCube Collaboration
|journal=Physical Review Letters |volume=113 |issue=10 |pages=101101 |arxiv=1405.5303 |bibcode=2014PhRvL.113j1101A |last1=Aartsen |first1=M. G. |s2cid=220469354 |display-authors=etal}}</ref> making such a distinction impossible.
Another type of indirect WIMP signal could come from the Sun. Halo WIMPs may, as they pass through the Sun, interact with solar protons, helium nuclei as well as heavier elements. If a WIMP loses enough energy in such an interaction to fall below the local [[escape velocity]], it would theoretically not have enough energy to escape the gravitational pull of the Sun and would remain gravitationally bound.<ref name="Griest" /> As more and more WIMPs thermalize inside the Sun, they would begin to [[annihilation|annihilate]] with each other, theoretically forming a variety of particles, including high-energy [[neutrino]]s.<ref>{{cite journal |doi=10.1103/PhysRevD.74.115007 |title=Indirect detection of light neutralino dark matter in the next-to-minimal supersymmetric standard model |date=2006 |last1=Ferrer |first1=F. |last2=Krauss |first2=L. M. |last3=Profumo |first3=S. |journal=Physical Review D |volume=74 |issue=11 |pages=115007 |arxiv=hep-ph/0609257 |bibcode=2006PhRvD..74k5007F |s2cid=119351935 }}</ref> These neutrinos may then travel to the Earth to be detected in one of the many neutrino telescopes, such as the [[Super-Kamiokande]] detector in Japan. The number of neutrino events detected per day at these detectors depends on the properties of the WIMP, as well as on the mass of the [[Higgs boson]]. Similar experiments are underway to attempt to detect neutrinos from WIMP annihilations within the Earth<ref>{{cite journal |doi=10.1016/0370-2693(86)90349-7|title=Can scalar neutrinos or massive Dirac neutrinos be the missing mass?|journal=Physics Letters B|volume=167|issue=3|pages=295–300|year=1986|last1=Freese|first1=Katherine|bibcode=1986PhLB..167..295F}}</ref> and from within the galactic center.<ref>{{cite journal |doi=10.1142/S0217732305017391 |title=Dark Matter Dynamics and Indirect Detection |date=2005 |last1=Merritt |first1=D. |last2=Bertone |first2=G. |author-link=David Merritt |journal=Modern Physics Letters A |volume=20 |issue=14 |pages=1021–1036 |arxiv=astro-ph/0504422 |bibcode=2005MPLA...20.1021B |s2cid=119405319 }}</ref><ref>{{
== Direct detection ==
{{see also|Direct detection of dark matter}}
''Direct detection'' refers to the observation of the effects of a WIMP-nucleus collision as the dark matter passes through a detector in an Earth laboratory. While most WIMP models indicate that a large enough number of WIMPs must be captured in large celestial bodies for indirect detection experiments to succeed, it remains possible that these models are either incorrect or only explain part of the dark matter phenomenon. Thus, even with the multiple experiments dedicated to providing indirect evidence for the existence of cold dark matter, direct detection measurements are also necessary to solidify the theory of WIMPs.
Although most WIMPs encountering the Sun or the Earth are expected to pass through without any effect, it is hoped that a large number of dark matter WIMPs crossing a sufficiently large detector will interact often enough to be seen—at least a few events per year. The general strategy of current attempts to detect WIMPs is to find very sensitive systems that can be scaled
[[Image:CDMS parameter space 2004.png |thumb|right
=== Experimental techniques ===
'''Cryogenic crystal detectors''' – A technique used by the [[Cryogenic Dark Matter Search]] (CDMS) detector at the [[Soudan Mine]] relies on multiple very cold germanium and silicon crystals. The crystals (each about the size of a hockey puck) are cooled to about 50 [[Kelvin|mK]]. A layer of metal (aluminium and tungsten) at the surfaces is used to detect a WIMP passing through the crystal. This design hopes to detect vibrations in the crystal matrix generated by an atom being "kicked" by a WIMP. The tungsten [[transition edge sensors]] (TES) are held at the critical temperature so they are in the [[superconducting]] state. Large crystal vibrations will generate heat in the metal and are detectable because of a change in [[electrical resistance|resistance]]. [[Cryogenic Rare Event Search with Superconducting Thermometers|CRESST]], [[CoGeNT]], and [[EDELWEISS]] run similar setups.
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'''Noble gas scintillators''' – Another way of detecting atoms "knocked about" by a WIMP is to use [[scintillator|scintillating]] material, so that light pulses are generated by the moving atom and detected, often with PMTs. Experiments such as [[DEAP]] at [[SNOLAB]] and [[DarkSide (dark matter experiment)|DarkSide]] at the [[Laboratori Nazionali del Gran Sasso|LNGS]] instrument a very large target mass of liquid argon for sensitive WIMP searches. [[ZEPLIN]], and [[XENON Dark Matter Search Experiment|XENON]] used xenon to exclude WIMPs at higher sensitivity, with the most stringent limits to date provided by the XENON1T detector, utilizing 3.5 tons of liquid xenon.<ref>{{cite journal |arxiv=1705.06655 |last1=Aprile|first1=E|display-authors=etal |title=First Dark Matter Search Results from the XENON1T Experiment |journal=Physical Review Letters|volume=119|issue=18|pages=181301|year=2017|doi=10.1103/PhysRevLett.119.181301|pmid=29219593|bibcode=2017PhRvL.119r1301A|s2cid=45532100}}</ref> Even larger multi-ton liquid xenon detectors have been approved for construction from the [[XENON]], [[LUX-ZEPLIN]] and [[PandaX]] collaborations.
'''Crystal scintillators''' – Instead of a liquid noble gas, an in principle simpler approach is the use of a scintillating crystal such as NaI(Tl). This approach is taken by [[DAMA/LIBRA]], an experiment that observed an annular modulation of the signal consistent with WIMP detection (see ''{{section link||Recent limits}}''). Several experiments are attempting to replicate those results, including [[ANAIS]], [[Cryogenic_Observatory_for_Signatures_Seen_in_Next-Generation_Underground_Searches|COSINUS]] and [[DM-Ice]], which is codeploying NaI crystals with the [[IceCube Neutrino Observatory|IceCube]] detector at the South Pole. [[Korea Invisible Mass Search|KIMS]] is approaching the same problem using CsI(Tl) as a scintillator.
'''Bubble chambers''' – The [[PICASSO]] (Project In Canada to Search for Supersymmetric Objects) experiment is a direct dark matter search experiment that is located at [[SNOLAB]] in Canada. It uses bubble detectors with [[Freon]] as the active mass. PICASSO is predominantly sensitive to spin-dependent interactions of WIMPs with the fluorine atoms in the Freon. COUPP, a similar experiment using trifluoroiodomethane(CF<sub>3</sub>I), published limits for mass above 20
A bubble detector is a radiation sensitive device that uses small droplets of superheated liquid that are suspended in a gel matrix.<ref>
PICASSO reports results (November 2009) for spin-dependent WIMP interactions on <sup>19</sup>F, for masses of 24 Gev new stringent limits have been obtained on the spin-dependent cross section of 13.9 pb (90% CL). The obtained limits restrict recent interpretations of the DAMA/LIBRA annual modulation effect in terms of spin dependent interactions.<ref>{{cite journal |author=PICASSO Collaboration |title=Dark Matter Spin-Dependent Limits for WIMP Interactions on <sup>19</sup>F by PICASSO |journal=Physics Letters B |date=2009 |doi=10.1016/j.physletb.2009.11.019 |bibcode=2009PhLB..682..185A |volume=682 |issue=2 |pages=185–192 |arxiv=0907.0307|s2cid=15163629 }}</ref>
PICO is an expansion of the concept planned in 2015.<ref>{{
'''Other types of detectors''' – [[Time projection chamber]]s (TPCs) filled with low pressure gases are being studied for WIMP detection. The [[Directional Recoil Identification From Tracks]] (DRIFT) collaboration is attempting to utilize the predicted directionality of the WIMP signal. DRIFT uses a [[carbon disulfide]] target, that allows WIMP recoils to travel several millimetres, leaving a track of charged particles. This charged track is drifted to an [[MWPC]] readout plane that allows it to be reconstructed in three dimensions and determine the origin direction. DMTPC is a similar experiment with CF<sub>4</sub> gas.
The DAMIC (DArk Matter In CCDs)
=== Recent limits ===
[[File:Direct Detection Constraints.png |
There are currently no confirmed detections of dark matter from direct detection experiments, with the strongest exclusion limits coming from the [[Large Underground Xenon experiment|LUX]] and [[Cryogenic Dark Matter Search|SuperCDMS]] experiments, as shown in figure 2.
With 370 kilograms of xenon, LUX is more sensitive than XENON or CDMS.<ref>
{{cite web |url=https://www.science.org/content/article/new-experiment-torpedoes-lightweight-dark-matter-particles |title=New Experiment Torpedoes Lightweight Dark Matter Particles |date=30 October 2013 |access-date=6 May 2014}}
</ref>
{{cite web |url=http://newscenter.lbl.gov/news-releases/2013/10/30/lux-first-results/ |title=First Results from LUX, the World's Most Sensitive Dark Matter Detector |publisher=Berkeley Lab News Center |date=30 October 2013 |access-date=6 May 2014}}
</ref>
Historically, there have been four anomalous sets of data from different direct detection experiments, two of which have now been explained with backgrounds ([[CoGeNT]] and CRESST-II), and two which remain unexplained ([[DAMA/LIBRA]] and [[Cryogenic Dark Matter Search|CDMS-Si]]).<ref>{{cite journal |title=Largest-ever dark-matter experiment poised to test popular theory |url=http://www.nature.com/news/largest-ever-dark-matter-experiment-poised-to-test-popular-theory-1.18772 |journal=Nature |access-date=15 January 2017|doi=10.1038/nature.2015.18772 |year=2015 |last1=Cartlidge |first1=Edwin |s2cid=182831370 |url-access=subscription }}</ref><ref>{{cite journal |last1=Davis |first1=Jonathan H. |date=2015 |title=The Past and Future of Light Dark Matter Direct Detection |journal=
{{cite web
|url = http://cdms.berkeley.edu/0912.3592v1.pdf
|title = Results from the Final Exposure of the CDMS II Experiment
|author = CDMS Collaboration
|access-date = 2009-12-21
}}. See also a non-technical summary: {{Cite web▼
|archive-date = 2009-12-29
|url = http://cdms.berkeley.edu/results_summary.pdf▼
|archive-url = https://web.archive.org/web/20091229234000/http://cdms.berkeley.edu/0912.3592v1.pdf
|title = Latest Results in the Search for Dark Matter▼
|
|url-status = dead▼
{{cite web
▲ |url = http://cdms.berkeley.edu/results_summary.pdf
▲ |title = Latest Results in the Search for Dark Matter
|author = CDMS Collaboration
|archive-url = https://web.archive.org/web/20100618221140/http://cdms.berkeley.edu/results_summary.pdf
|archive-date = 2010-06-18
}}</ref><ref>{{cite journal |author=The CDMS II Collaboration |date=2010 |title=Dark Matter Search Results from the CDMS II Experiment |journal=Science
[[CoGeNT]], a smaller detector using a single germanium puck, designed to sense WIMPs with smaller masses, reported hundreds of detection events in 56 days.<ref name="NN-2010-02-26">{{cite journal |author=Hand |first=Eric |date=2010-02-26 |title=A CoGeNT result in the hunt for dark matter |url=http://www.nature.com/news/2010/100226/full/news.2010.97.html
Annual modulation is one of the predicted signatures of a WIMP signal,<ref>{{cite journal|last1=Drukier|first1=Andrzej K.|last2=Freese|first2=Katherine|last3=Spergel|first3=David N.|title=Detecting cold dark-matter candidates|journal=Physical Review D|date=15 June 1986|volume=33|issue=12|pages=3495–3508|doi=10.1103/PhysRevD.33.3495|pmid=9956575|bibcode=1986PhRvD..33.3495D}}</ref><ref name="Freese1988">{{cite journal |author=Freese |first1=K.
The [[Korea Invisible Mass Search#COSINE|COSINE-100]] collaboration (a merging of KIMS and DM-Ice groups) published their results on replicating the DAMA/LIBRA signal in December 2018 in journal Nature; their conclusion was that "this result rules out WIMP–nucleon interactions as the cause of the annual modulation observed by the DAMA collaboration".<ref>{{
===
[[File:
The 2020s should see the emergence of several multi-tonne mass direct detection experiments, which will probe WIMP-nucleus cross sections orders of magnitude smaller than the current state-of-the-art sensitivity. Examples of such next-generation experiments are LUX-ZEPLIN (LZ) and XENONnT, which are multi-tonne liquid xenon experiments, followed by DARWIN, another proposed liquid xenon direct detection experiment of 50–100 tonnes.<ref>{{cite arXiv |eprint=1110.0103|last1= Malling|first1= D. C.|title= After LUX: The LZ Program |display-authors= etal |class= astro-ph.IM|year= 2011}}</ref><ref>{{cite journal |last1=Baudis |first1=Laura |title=DARWIN: dark matter WIMP search with noble liquids |journal=J. Phys. Conf. Ser. |date=2012 |volume=375 |issue=1 |page=012028 |doi=10.1088/1742-6596/375/1/012028 |arxiv=1201.2402|bibcode=2012JPhCS.375a2028B |s2cid=30885844 }}</ref>
Such multi-tonne experiments will also face a new background in the form of neutrinos, which will limit their ability to probe the WIMP parameter space beyond a certain point, known as the neutrino floor. However, although its name may imply a hard limit, the neutrino floor represents the region of parameter space beyond which experimental sensitivity can only improve at best as the square root of exposure (the product of detector mass and running time).<ref>{{cite journal |last1=Billard |first1=J. |last2=Strigari |first2=L. |last3=Figueroa-Feliciano |first3=E. |date=2014 |title=Implication of neutrino backgrounds on the reach of next generation dark matter direct detection experiments |journal=
In December 2021, results from [[PandaX]] have found no signal in their data, with a lowest excluded cross section of
In July 2023, the [[XENON#XENONnT|XENONnT]] and [[LZ experiment]] published the first results of their searches for WIMPs,<ref>{{cite journal |last=Day |first=Charles |date=2023-07-28 |title=The Search for WIMPs Continues |url=https://physics.aps.org/articles/v16/s106 |journal=Physics |volume=16 |pages=s106 |doi=10.1103/Physics.16.s106 |bibcode=2023PhyOJ..16.s106D |s2cid=260751963 |language=en |doi-access=free }}</ref> the first excluding cross sections above {{val|2.58|e=-47|u=cm2}} at 28 GeV with 90% confidence level<ref>{{cite journal |last1=XENON Collaboration |last2=Aprile |first2=E. |last3=Abe |first3=K. |last4=Agostini |first4=F. |last5=Ahmed Maouloud |first5=S. |last6=Althueser |first6=L. |last7=Andrieu |first7=B. |last8=Angelino |first8=E. |last9=Angevaare |first9=J. R. |last10=Antochi |first10=V. C. |last11=Antón Martin |first11=D. |last12=Arneodo |first12=F. |last13=Baudis |first13=L. |last14=Baxter |first14=A. L. |last15=Bazyk |first15=M. |date=2023-07-28 |title=First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment |url=https://link.aps.org/doi/10.1103/PhysRevLett.131.041003 |journal=Physical Review Letters |volume=131 |issue=4 |pages=041003 |doi=10.1103/PhysRevLett.131.041003|pmid=37566859 |arxiv=2303.14729 |bibcode=2023PhRvL.131d1003A |s2cid=257767449 }}</ref> and the second excluding cross sections above {{val|9.2|e=-48|u=cm2}} at 36 GeV with 90% confidence level.<ref>{{cite journal |last1=LUX-ZEPLIN Collaboration |last2=Aalbers |first2=J. |last3=Akerib |first3=D. S. |last4=Akerlof |first4=C. W. |last5=Al Musalhi |first5=A. K. |last6=Alder |first6=F. |last7=Alqahtani |first7=A. |last8=Alsum |first8=S. K. |last9=Amarasinghe |first9=C. S. |last10=Ames |first10=A. |last11=Anderson |first11=T. J. |last12=Angelides |first12=N. |last13=Araújo |first13=H. M. |last14=Armstrong |first14=J. E. |last15=Arthurs |first15=M. |date=2023-07-28 |title=First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment |url=https://link.aps.org/doi/10.1103/PhysRevLett.131.041002 |journal=Physical Review Letters |volume=131 |issue=4 |pages=041002 |doi=10.1103/PhysRevLett.131.041002|pmid=37566836 |arxiv=2207.03764 |bibcode=2023PhRvL.131d1002A |s2cid=250343331 }}</ref>
==See also==▼
▲== See also ==
<!-- Please keep entries in alphabetical order & add a short description [[WP:SEEALSO]] -->
{{
* {{annotated link|Darkon (unparticle)}}
* [[Feebly Interacting Particles|Feebly interacting particle]] (FIP)
*{{annotated link|Higgs boson}}▼
* {{annotated link|Higgs boson}}
* {{annotated link|Massive compact halo object|abbreviation=MACHO}} * {{annotated link|Micro black hole}}
* {{annotated link|Robust associations of massive baryonic objects|abbreviation=RAMBOs}}
* [[WISP (particle physics)|Weakly
{{div col end}}
*Theoretical candidates▼
**{{annotated link|Lightest supersymmetric particle|abbreviation=LSP}}▼
**{{annotated link|Neutralino}}▼
{{div col begin|colwidth=20em}}
**{{annotated link|Micro black hole#Conjectures for the final state|Planck-mass-sized black hole remnant}}▼
*
▲*
{{div col end}}
<!-- please keep entries in alphabetical order -->
== References ==
{{reflist}}
== Further reading ==
* {{
|last=Bertone
|first=Gianfranco
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|bibcode=2010pdmo.book.....B
}}
* {{
* {{cite journal |last1=Davis |first1=Jonathan H. |title=The Past and Future of Light Dark Matter Direct Detection |journal=
* {{cite journal |title=Update on the Halo-independent Comparison of Direct Dark Matter Detection Data |year=2015 |journal=Physics Procedia |doi=10.1016/j.phpro.2014.12.009 |volume=61 |pages=45–54 |last1=Del Nobile |first1=Eugenio |last2=Gelmini |first2=Graciela B. |last3=Gondolo |first3=Paolo |last4=Huh |first4=Ji-Haeng |bibcode=2015PhPro..61...45D |arxiv = 1405.5582 }}
== External links ==
* [http://pdg.lbl.gov/2004/listings/s030.pdf Particle Data Group review article on WIMP search] (S. Eidelman et al. (Particle Data Group),
* [[Timothy J. Sumner]], [https://web.archive.org/web/20061020063709/http://relativity.livingreviews.org/Articles/lrr-2002-4/index.html Experimental Searches for Dark Matter] in Living Reviews in Relativity, Vol 5, 2002.
* [https://www.newscientist.com/article/mg21929320.700-out-of-the-shadows-picking-up-hints-of-dark-matter.html Portraits of darkness, New Scientist, August 31, 2013. Preview only.]
* {{
{{Dark matter}}
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