Weakly interacting massive particle: Difference between revisions

Revision as of 00:37, 23 December 2023

Revision as of 00:51, 23 December 2023

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===Recent limits===

[[File:Direct Detection Constraints.png |frame|Fig.Figure 2: Plot showing the parameter space of dark matter particle mass and interaction cross section with nucleons. The LUX and SuperCDMS limits exclude the parameter space above the labelled curves. The CoGeNT and CRESST-II regions indicate regions which were previously thought to correspond to dark matter signals, but which were later explained with mundane sources. The DAMA and CDMS-Si data remain unexplained, and these regions indicate the preferred parameter space if these anomalies are due to dark matter.]]

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.

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</ref> and this was confirmed after the final data run ended in May 2016.<ref>[https://www.science.org/content/article/dark-matter-search-comes-empty Dark matter search comes up empty. July 2016]</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 }}</ref><ref>{{cite journal |last1=Davis |first1=Jonathan H. |date=2015 |title=The Past and Future of Light Dark Matter Direct Detection |journal=Int.International J.Journal Mod.of Phys.Modern Physics A |date=2015 |volume=30 |issue=15 |page=1530038 |arxiv=1506.03924 |bibcode=2015IJMPA..3030038D |doi=10.1142/S0217751X15300380 |arxivs2cid=1506119269304}}</ref> In February 2010, researchers at CDMS announced that they had observed two events that may have been caused by WIMP-nucleus collisions.03924<ref name="strib">{{cite web |bibcodeurl=2015IJMPAhttp://www.startribune.3030038Dcom/local/79624932.html?page=1&c=y |s2cidtitle=119269304Key to the universe found on the Iron Range? |website=[[Star Tribune]] |access-date=December 18, 2009}}</ref><ref>{{Cite web

In February 2010, researchers at CDMS announced that they had observed two events that may have been caused by WIMP-nucleus collisions.<ref name="strib">{{cite web |url=http://www.startribune.com/local/79624932.html?page=1&c=y |title=Key to the universe found on the Iron Range? |website=[[Star Tribune]] |access-date=December 18, 2009}}</ref><ref>{{Cite web

|url = http://cdms.berkeley.edu/0912.3592v1.pdf

|title = Results from the Final Exposure of the CDMS II Experiment

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|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 |date=2010 |doi=10.1126/science.1186112 |pmid=20150446 |volume=327 |issue=5973 |pages=1619–211619–1621 |arxiv=0912.3592 |bibcode=2010Sci...327.1619C |doi=10.1126/science.1186112 |pmid=20150446 |s2cid=2517711 }}</ref>

[[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 |title=A CoGeNT result in the hunt for dark matter |journal=Nature |author=Eric Hand |publisher=Nature News |date=2010-02-26|doi=10.1038/news.2010.97 }}</ref><ref>{{cite journal |title=Results from a Search for Light-Mass Dark Matter with a P-type Point Contact Germanium Detector |author=C. E. Aalseth |collaboration=CoGeNT collaboration |doi=10.1103/PhysRevLett.106.131301 |date=2011 |journal=Physical Review Letters |volume=106 |issue=13 |arxiv=1002.4703 |bibcode=2011PhRvL.106m1301A |pmid=21517370 |page=131301|s2cid=24822628 }}</ref> They observed an annual modulation in the event rate that could indicate light dark matter.<ref name="Dacey2011">{{cite web |last1=Dacey |first=James Dacey|date=June 2011 |title=CoGeNT findings support dark-matter halo theory |url=http://physicsworld.com/cws/article/news/2011/jun/15/cogent-findings-support-dark-matter-halo-theory |publisher=physicsworld |date=June 2011 |access-date=5 May 2015 |publisher=physicsworld}}</ref> However a dark matter origin for the CoGeNT events has been refuted by more recent analyses, in favour of an explanation in terms of a background from surface events.<ref>{{cite journal |last1=Davis |first1=Jonathan H. |last2=McCabe |first2=Christopher |last3=Boehm |first3=Celine |title=Quantifying the evidence for Dark Matter in CoGeNT data |journal=Journal of Cosmology and Astroparticle Physics |date=2014 |volume=1408 |issue=8 |page=014 |doi=10.1088/1475-7516/2014/08/014 |arxiv = 1405.0495 |bibcode = 2014JCAP...08..014D |s2cid=54532870 }}</ref>

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 |first=K. Freese |author2=Frieman |first2=J. Frieman |author3=Gould |first3=A. Gould|year=1988 |title=Signal Modulation in Cold Dark Matter Detection |journal=Physical Review D |year=1988 |doi=10.1103/PhysRevD.37.3388 |pmid=9958634 |volume=37 |issue=12 |pages=3388–3405 |bibcode = 1988PhRvD..37.3388F |doi=10.1103/PhysRevD.37.3388 |osti=1448427 |pmid=9958634 |s2cid=2610174 }}</ref> and on this basis the DAMA collaboration has claimed a positive detection. Other groups, however, have not confirmed this result. The CDMS data made public in May 2004 exclude the entire DAMA signal region given certain standard assumptions about the properties of the WIMPs and the dark matter halo, and this has been followed by many other experiments (see FigFigure 2, right).

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>{{Cite journal | doi=10.1038/s41586-018-0739-1|pmid = 30518890| title=An experiment to search for dark-matter interactions using sodium iodide detectors| journal=Nature| volume=564| issue=7734| pages=83–86| year=2018| author1=COSINE-100 Collaboration| bibcode=2018Natur.564...83C|arxiv = 1906.01791|s2cid = 54459495}}</ref> In 2021 new results from COSINE-100 and [[ANAIS-112]] both failed to replicate the DAMA/LIBRA signal<ref>{{Cite journal |last1=Amaré |first1=J. |last2=Cebrián |first2=S. |last3=Cintas |first3=D. |last4=Coarasa |first4=I. |last5=García |first5=E. |last6=Martínez |first6=M. |last7=Oliván |first7=M. A. |last8=Ortigoza |first8=Y. |last9=de Solórzano |first9=A. Ortiz |last10=Puimedón |first10=J. |last11=Salinas |first11=A. |date=2021-05-27 |title=Annual modulation results from three-year exposure of ANAIS-112 |url=https://link.aps.org/doi/10.1103/PhysRevD.103.102005 |journal=Physical Review D |language=en |volume=103 |issue=10 |pages=102005 |arxiv=2103.01175 |bibcode=2021PhRvD.103j2005A |doi=10.1103/PhysRevD.103.102005 |issn=2470-0010 |s2cid=232092298}}</ref><ref>{{Cite journal |last1=Adhikari |first1=Govinda |last2=de Souza |first2=Estella B. |last3=Carlin |first3=Nelson |last4=Choi |first4=Jae Jin |last5=Choi |first5=Seonho |last6=Djamal |first6=Mitra |last7=Ezeribe |first7=Anthony C. |last8=França |first8=Luis E. |last9=Ha |first9=Chang Hyon |last10=Hahn |first10=In Sik |last11=Jeon |first11=Eunju |date=2021-11-12 |title=Strong constraints from COSINE-100 on the DAMA dark matter results using the same sodium iodide target |journal=Science Advances |language=en |volume=7 |issue=46 |pages=eabk2699 |bibcode=2021SciA....7.2699A |doi=10.1126/sciadv.abk2699 |issn=2375-2548 |pmc=8580298 |pmid=34757778|arxiv=2104.03537 }}</ref><ref>{{Cite web |title=Is the end in sight for famous dark matter claim? |url=https://www.science.org/content/article/end-sight-famous-dark-matter-claim |access-date=2021-12-29 |website=www.science.org |language=en}}</ref> and in August 2022 COSINE-100 applied an analysis method similar to one used by DAMA/LIBRA and found a similar annual modulation suggesting the signal could be just a statistical artifact<ref>{{cite journal |last1=Adhikari |first1=G. |last2=Carlin |first2=N. |last3=Choi |first3=J. J. |last4=Choi |first4=S. |last5=Ezeribe |first5=A. C. |last6=Franca |first6=L. E. |last7=Ha |first7=C. |last8=Hahn |first8=I. S. |last9=Hollick |first9=S. J. |last10=Jeon |first10=E. J. |last11=Jo |first11=J. H. |last12=Joo |first12=H. W. |last13=Kang |first13=W. G. |last14=Kauer |first14=M. |last15=Kim |first15=B. H. |date=2023 |title=An induced annual modulation signature in COSINE-100 data by DAMA/LIBRA's analysis method |journal=Scientific Reports |volume=13 |issue=1 |page=4676 |doi=10.1038/s41598-023-31688-4 |pmid=36949218 |pmc=10033922 |arxiv=2208.05158 |bibcode=2023NatSR..13.4676A }}</ref><ref>{{Cite journal |last=Castelvecchi |first=Davide |date=2022-08-16 |title=Notorious dark-matter signal could be due to analysis error |url=https://www.nature.com/articles/d41586-022-02222-9 |journal=Nature |language=en |doi=10.1038/d41586-022-02222-9|pmid=35974221 |s2cid=251624302 }}</ref> supporting a hypothesis first put forward on 2020.<ref>{{cite journal |author=Buttazzo |first=D. Buttazzo |display-authors=etal |year=2020 |title=Annual modulations from secular variations: relaxing DAMA? |journal=Journal of High Energy Physics |volume=2020 |issue=4 |page=137 |arxiv=2002.00459 |bibcode=2020JHEP...04..137B |doi=10.1007/JHEP04(2020)137 |s2cid=211010848}}</ref>

===The future of direct detection===

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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=Phys.Physical Rev.Review D |date=2014 |volume=89 |issue=2 |page=023524 |doi=10.1103/PhysRevD.89.023524 |arxiv=1307.5458 |bibcode = 2014PhRvD..89b3524B |doi=10.1103/PhysRevD.89.023524 |s2cid=16208132 }}</ref><ref>{{cite journal |last1=Davis |first1=Jonathan H. |title=Dark Matter vs. Neutrinos: The effect of astrophysical uncertainties and timing information on the neutrino floor |journal=Journal of Cosmology and Astroparticle Physics |date=2015 |volume=1503 |issue=3 |page=012 |doi=10.1088/1475-7516/2015/03/012 |arxiv=1412.1475|bibcode = 2015JCAP...03..012D |s2cid=118596203 }}</ref> For WIMP masses below 10 GeV the dominant source of neutrino background is from the [[Solar neutrino|Sun]], while for higher masses the background contains contributions from [[Neutrino#Atmospheric|atmospheric neutrino]]s and the [[diffuse supernova neutrino background]].

In December 2021, results from [[PandaX]] have found no signal in their data, with a lowest excluded cross section of <math>3.8\times10^{-47} cm^2</math> at 40 GeV with 90% confidence level.<ref name="Meng et al-2021">{{Cite journal|last1=Meng|first1=Yue|last2=Wang|first2=Zhou|last3=Tao|first3=Yi|last4=Abdukerim|first4=Abdusalam|last5=Bo|first5=Zihao|last6=Chen|first6=Wei|last7=Chen|first7=Xun|last8=Chen|first8=Yunhua|last9=Cheng|first9=Chen|last10=Cheng|first10=Yunshan|last11=Cui|first11=Xiangyi|date=2021-12-23|title=Dark Matter Search Results from the PandaX-4T Commissioning Run|url=https://link.aps.org/doi/10.1103/PhysRevLett.127.261802|journal=Physical Review Letters|language=en|volume=127|issue=26|pages=261802|doi=10.1103/PhysRevLett.127.261802|pmid=35029500| arxiv=2107.13438 | bibcode=2021PhRvL.127z1802M |s2cid=236469421|issn=0031-9007}}</ref><ref name="Stephens-2021">{{Cite journal|last=Stephens|first=Marric|date=2021-12-23|title=Tightening the Net on Two Kinds of Dark Matter|url=https://physics.aps.org/articles/v14/s164|journal=Physics|language=en|volume=14| doi=10.1103/Physics.14.s164 | bibcode=2021PhyOJ..14.s164S | s2cid=247277808 |doi-access=free}}</ref>

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}}

*{{Cite journal |last1=Cerdeño |first1=David G. |last2=Green |first2=Anne M. |editor1-first=Gianfranco |editor1-last=Bertone |title=Direct detection of WIMPs |journal=Particle Dark Matter: Observations, Models and Searches |date=2010 |pages=347–369 |arxiv=1002.1912 |doi=10.1017/CBO9780511770739.018|isbn=9780511770739 |s2cid=119311963 }}

*{{cite journal |last1=Davis |first1=Jonathan H. |title=The Past and Future of Light Dark Matter Direct Detection |journal=Int.International J.Journal Mod.of Phys.Modern Physics A |date=2015 |volume=30 |issue=15 |page=1530038 |doi=10.1142/S0217751X15300380 |arxiv=1506.03924 |bibcode=2015IJMPA..3030038D |s2cid=119269304 }}

*{{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), Phys.Physical Lett.Letters B 592, 1 (2004) Appendix : OMITTED FROM SUMMARY TABLE).

*[[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.]

*{{Cite AV media|url=https://www.youtube.com/watch?v=3YMWHkFW5VA |archive-url=https://ghostarchive.org/varchive/youtube/20211211/3YMWHkFW5VA| archive-date=2021-12-11 |url-status=live|title=The WIMP is dead. Long live the WIMP!|date=13 April 2018|last=Hooper|first=Dan|type=video; colloquium|publisher=Brown University Department of Physics|author-link=Dan Hooper}}{{cbignore}}