120:. The prompt scintillation light produces 178 nm ultraviolet photons. This signal is detected by the PMTs, and is referred to as the S1 signal. The applied electric field prevents recombination of all the electrons produced from a charged particle interaction in the TPC. These electrons are drifted to the top of the liquid phase by the electric field. The ionization is then extracted into the gas phase by the stronger electric field in the gaseous phase. The electric field accelerates the electrons to the point that it creates a proportional scintillation signal that is also collected by the PMTs, and is referred to as the S2 signal. This technique has proved sensitive enough to detect S2 signals generated from single electrons.
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used as a discrimination parameter to distinguish electronic and nuclear recoil events. This ratio is expected to be greater for electronic recoils than for nuclear recoils. In this way backgrounds from electronic recoils can be suppressed by more than 99%, while simultaneously retaining 50% of the nuclear recoil events.
376:
XENONnT is an upgrade of the XENON1T experiment underground at LNGS. Its systems will contain a total xenon mass of more than 8 tonnes. Apart from a larger xenon target in its time projection chamber the upgraded experiment will feature new components to further reduce or tag radiation that otherwise
132:
Charged particles moving through the detector are expected to either interact with the electrons of the xenon atoms producing electronic recoils, or with the nucleus, producing nuclear recoils. For a given amount of energy deposited by a particle interaction in the detector, the ratio of S2/S1 can be
128:
of the detector, in which a low-background region is defined in the inner volume of the TPC. This fiducial volume has a greatly reduced rate of background events as compared to regions of the detector at the edge of the TPC, due to the self-shielding properties of liquid xenon. This allows for a much
380:
The XENONnT detector was under construction in March 2020. Even with the problems posed by COVID-19, the project was able to finish construction and move forwards into commissioning phase by mid 2020. Full detector operations commenced in late 2020. In
September 2021, XENONnT was taking science data
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WIMP mass. These results constrain interpretations of signals in other experiments as dark matter interactions, and rule out exotic models such as inelastic dark matter, which would resolve this discrepancy. XENON100 has also provided improved limits on the spin dependent WIMP-nucleon cross section.
214:
The second phase detector, XENON100, contains 165 kg of liquid xenon, with 62 kg in the target region and the remaining xenon in an active veto. The TPC of the detector has a diameter of 30 cm and a height of 30 cm. As WIMP interactions are expected to be extremely rare events, a
158:
during March 2006. The underground location of the laboratory provides 3100 m of water-equivalent shielding. The detector was placed within a shield to further reduce the background rate in the TPC. XENON10 was intended as a prototype detector, to prove the efficacy of the XENON design, as well
162:
An analysis of 59 live days of data, taken between
October 2006 and February 2007, produced no WIMP signatures. The number of events observed in the WIMP search region is statistically consistent with the expected number of events from electronic recoil backgrounds. This result excluded some of the
123:
The detector allows for a full 3-D position determination of the particle interaction. Electrons in liquid xenon have a uniform drift velocity. This allows the interaction depth of the event to be determined by measuring the time delay between the S1 and S2 signal. The position of the event in the
334:
in xenon-124 nuclei. The measured half-life of this process, which is several orders of magnitude larger than the age of the
Universe, demonstrates the capabilities of xenon-based detectors to search for rare events and showcases the broad physics reach of even larger next-generation experiments.
281:
The first results from XENON1T were released by the XENON collaboration on May 18, 2017, based on 34 days of data-taking between
November 2016 and January 2017. While no WIMPs or dark matter candidate signals were officially detected, the team did announce a record low reduction in the background
185:
Due to nearly half of natural xenon having odd spin states (Xe has an abundance of 26% and spin-1/2; Xe has an abundance of 21% and spin-3/2), the XENON detectors can also be used to provide limits on spin dependent WIMP-nucleon cross sections for coupling of the dark matter candidate particle to
67:
signals produced when external particles interact in the liquid xenon volume, to search for an excess of nuclear recoil events against known backgrounds. The detection of such a signal would provide the first direct experimental evidence for dark matter candidate particles. The collaboration is
230:
in 2008 in the same shield as the XENON10 detector, and has conducted several science runs. In each science run, no dark matter signal was observed above the expected background, leading to the most stringent limit on the spin independent WIMP-nucleon cross section in 2012, with a minimum at
108:
light produced when charged particles interact in the detector. Electric fields are applied across both the liquid and gaseous phase of the detector. The electric field in the gaseous phase has to be sufficiently large to extract electrons from the liquid phase.
377:
would constitute background to its measurements. It is designed to reach a sensitivity (in a small part of the mass-range probed) where neutrinos become a significant background. As of 2019, the upgrade was on-going and first light was expected in 2020.
1962:
LUX-ZEPLIN Collaboration; Aalbers, J.; Akerib, D. S.; Akerlof, C. W.; Al
Musalhi, A. K.; Alder, F.; Alqahtani, A.; Alsum, S. K.; Amarasinghe, C. S.; Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M. (2023-07-28).
266:
in 2014. The detector contains 3.2 tons of ultra radio-pure liquid xenon, and has a fiducial volume of about 2 tons. The detector is housed in a 10 m water tank that serves as a muon veto. The TPC is 1 m in diameter and 1 m in height.
1722:
Aprile, E.; Abe, K.; Agostini, F.; Maouloud, S. Ahmed; Althueser, L.; Andrieu, B.; Angelino, E.; Angevaare, J. R.; Antochi, V. C.; Martin, D. Antón; Arneodo, F. (2022-07-22). "Search for New
Physics in Electronic Recoil Data from XENONnT".
350:
In June 2020, the XENON1T collaboration reported an excess of electron recoils: 285 events, 53 more than the expected 232 with a statistical significance of 3.5σ. Three explanations were considered: existence of to-date-hypothetical solar
85:
1904:
XENON Collaboration; Aprile, E.; Abe, K.; Agostini, F.; Ahmed
Maouloud, S.; Althueser, L.; Andrieu, B.; Angelino, E.; Angevaare, J. R.; Antochi, V. C.; Antón Martin, D.; Arneodo, F.; Baudis, L.; Baxter, A. L.; Bazyk, M. (2023-07-28).
159:
as verify the achievable threshold, background rejection power and sensitivity. The XENON10 detector contained 15 kg of liquid xenon. The sensitive volume of the TPC measures 20 cm in diameter and 15 cm in height.
346:
As of 2019, the XENON1T experiment has stopped data-taking to allow for construction of the next phase, XENONnT. The XENON1T detector operated 2016–2018, with the detector operations ending at the end of 2018.
359:
for neutrinos, and tritium contamination in the detector. Multiple other explanations were given later by others groups and in 2021 an interpretation of the results not as dark matter particles but of as
145:
The cryostat and shield of XENON100. The shield consists of an outer layer of 20 cm of water, a 20 cm layer of lead, a 20 cm layer of polyethylene, and on the interior a 5 cm copper
308:
In
September 2018 the XENON1T experiment published its results from 278.8 days of collected data. A new record limit for WIMP-nucleon spin-independent elastic interactions was set, with a minimum of
2477:
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array of XENON100 contains 98 Hamamatsu R8520-06-A1 PMTs. The PMTs on the top array are placed in concentric circles to improve the reconstruction of the radial position of observed events.
431:
484:
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was performed on low mass plastic samples. In doing so the design goal of <10 events/kg/day/keV was reached, realising the world's lowest background rate dark matter detector.
215:
thorough campaign was launched during the construction and commissioning phase of XENON100 to screen all parts of the detector for radioactivity. The screening was performed using
2562:
2542:
1630:
Sunny
Vagnozzi; Luca Visinelli; Philippe Brax; Anne-Christine Davis; Jeremy Sakstein (2021). "Direct detection of dark energy: The XENON1T excess and future prospects".
270:
The detector project team, called the XENON Collaboration, is composed of 135 investigators across 22 institutions from Europe, the Middle East, and the United States.
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1819:
2136:
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2457:
1451:"Direct Dark Matter Search with XENONnT. International symposium on "Revealing the history of the Universe with underground particle and nuclear research""
2715:
732:
Angle, J.; et al. (XENON10 Collaboration) (2008). "First
Results from the XENON10 Dark Matter Experiment at the Gran Sasso National Laboratory".
502:
Aprile, E.; et al. (XENON100 Collaboration) (2014). "Observation and applications of single-electron charge signals in the XENON100 experiment".
1031:
Aprile, E.; et al. (XENON100 Collaboration) (2012). "Limits on spin-dependent WIMP-nucleon cross sections from 225 live days of XENON100 data".
2720:
2695:
1311:
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XENON100 operated the then-lowest background experiment, for dark matter searches, with a background of 50 mDRU (1 mDRU=10 events/kg/day/keV).
1684:
2312:
2187:
164:
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2400:
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Angle, J.; et al. (XENON10 Collaboration) (2008). "Limits on spin-dependent WIMP-nucleon cross-sections from the XENON10 experiment".
302:
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The bottom PMT array of XENON100 contains 80 PMTs which are spaced as closely as possible in order to maximize light collection efficiency.
45:
124:
x-y plane can be determined by looking at the number of photons seen by each of the individual PMTs. The full 3-D position allows for the
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2317:
263:
227:
151:
37:
2552:
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Aprile, E.; et al. (XENON100 Collaboration) (2011). "Implications on inelastic dark matter from 100 live days of XENON100 data".
283:
2507:
301:. Because some signals that the detector receives might be due to neutrons, reducing the radioactivity increases the sensitivity to
2292:
100:
tubes (PMTs), one at the top of the detector in the gaseous phase (GXe), and one at the bottom of the liquid layer (LXe), detect
2700:
2690:
2675:
2612:
1480:
1149:
Aprile, E.; et al. (XENON100 Collaboration) (2011). "Study of the electromagnetic background in the XENON100 experiment".
1605:
2820:
2023:
Angle, J; et al. (2008). "First Results from the XENON10 Dark Matter Experiment at the Gran Sasso National Laboratory".
1540:
2685:
2705:
2622:
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2452:
2447:
2432:
2242:
2660:
2547:
2487:
2467:
2390:
40:, is a deep underground detector facility featuring increasingly ambitious experiments aiming to detect hypothetical
913:
Aprile, E.; et al. (XENON100 Collaboration) (2012). "Dark Matter Results from 225 Live Days of XENON100 Data".
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radioactivity levels being picked up by XENON1T. The exclusion limits exceeded the previous best limits set by the
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2180:
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Upper limit for spin-independent WIMP-nucleon cross section according to recent data (published in November 2017)
384:
On 28 July 2023 the XENONnT published the first results of its search for WIMPs, excluding cross sections above
2405:
2247:
387:
1094:
Aprile, E.; et al. (XENON1000 Collaboration) (2014). "First Axion Results from the XENON100 Experiment".
440:
326:
In April 2019, based on measurements performed with the XENON1T detector, the XENON Collaboration reported in
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2025:
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1342:
1234:
1033:
915:
797:
734:
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Aprile, E.; et al. (XENON10 Collaboration) (2011). "Design and Performance of The XENON10 Experiment".
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331:
113:
101:
93:
60:
53:
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1768:
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Aprile, E.; et al. (XENON100 Collaboration) (2011). "Material screening and selection for XENON100".
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20:
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both neutrons and protons. XENON10 set the world's most stringent restrictions on pure neutron coupling.
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504:
199:
591:
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1494:
Aprile, E.; et al. (2020-06-17). "Observation of Excess Electronic Recoil Events in XENON1T".
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73:
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365:
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Aprile, E.; et al. (XENON100 Collaboration) (2012). "The XENON100 dark matter experiment".
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2002:
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96:(TPC), which utilizes a liquid xenon target with a gaseous phase on top. Two arrays of
368:
has also been discussed. In July 2022 a new analysis by XENONnT discarded the excess.
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718:
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1135:
1080:
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663:
622:
Aprile, E.; et al. (2014). "Analysis of the XENON100 dark matter search data".
608:
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1998:
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946:
828:
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167:, by placing limits on spin independent WIMP-nucleon cross sections down to below
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2287:
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2128:
1663:
1517:
1481:"Assembling the XENONnT Dark Matter Detector during Covid-19 Times » APPEC"
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41:
30:
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process, the detection of which would provide insight into the nature of the
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2746:
2537:
1848:
206:
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2006:
1948:
1907:"First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment"
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954:
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773:
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1685:
Have we detected dark energy? Cambridge scientists say it's a possibility
340:
194:
84:
2830:
2730:
2602:
1290:"The World's Most Sensitive Dark Matter Detector Is Now Up and Running"
2106:
1965:"First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment"
2587:
2462:
1698:"A new dark matter experiment quashed earlier hints of new particles"
1338:"Dark Matter Search Results from a One Ton-Year Exposure of XENON1T"
1312:"World's most sensitive dark matter detector releases first results"
1266:
1229:
48:(WIMPs) by looking for rare nuclear recoil interactions in a liquid
2096:
1981:
1923:
1865:
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638:
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at 28 GeV with 90% confidence level, jointly on the same date the
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272:
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Construction of the next phase, XENON1T, started in Hall B of the
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155:
83:
49:
44:
particles. The experiments aim to detect particles in the form of
34:
1606:"Excitement grows over mysterious signal in dark-matter detector"
2597:
2592:
2517:
2472:
2442:
2169:
437:
published its first results too excluding cross sections above
335:
This measurement represents a first step in the search for the
2165:
1230:"First Dark Matter Search Results from the XENON1T Experiment"
251:
result was published in 2014, setting a new best axion limit.
52:
target chamber. The current detector consists of a dual phase
2111:
2086:
1204:
381:
for its first science run, which was ongoing at the time.
88:
Sketch of the working principle of a xenon dual-phase TPC
2125:
with the latest results from XENON and other experiments
150:
The XENON10 experiment was installed at the underground
129:
higher sensitivity when searching for very rare events.
1820:"The XENONnT Experiment – Detector and Science Program"
1336:
Aprile, E.; et al. (XENON collaboration) (2018).
1228:
Aprile, E.; et al. (XENON collaboration) (2017).
443:
390:
1399:"Dark-matter detector observes exotic nuclear decay"
2798:
2764:
2739:
2651:
2423:
2414:
2331:
2270:
2203:
1769:"scanR | Moteur de la Recherche et de l'Innovation"
112:Particle interactions in the liquid target produce
478:
425:
286:, with an exclusion of cross sections larger than
2129:Enlightening the dark, CERN Courier, Sep 27, 2013
1541:"Dark Matter Experiment Finds Unexplained Signal"
1566:"Dark Matter Detector Delivers Enigmatic Signal"
68:currently led by Italian professor of physics
2181:
1475:
1473:
330:the first direct observation of two-neutrino
8:
2092:XENON home page at the University of Chicago
1687:, University of Cambridge, 15 September 2021
1205:"Homepage of the XENON1T Dark Matter Search"
2102:XENON home page at the University of Zurich
92:The XENON experiment operates a dual phase
2420:
2188:
2174:
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343:and allow to determine its absolute mass.
2038:
1980:
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426:{\displaystyle 2.58\times 10^{-47}cm^{2}}
417:
401:
389:
2119:at University of California, Los Angeles
479:{\displaystyle 9.2\times 10^{-48}cm^{2}}
205:
193:
140:
1773:scanr.enseignementsup-recherche.gouv.fr
494:
2097:XENON home page at Columbia University
1444:
1442:
486:at 36 GeV with 90% confidence level.
7:
2866:
337:neutrinoless double electron capture
46:weakly interacting massive particles
2112:XENON home page at Brown University
892:10.1016/j.astropartphys.2011.06.001
711:10.1016/j.astropartphys.2011.01.006
656:10.1016/j.astropartphys.2013.10.002
601:10.1016/j.astropartphys.2012.01.003
2894:Experiments for dark matter search
2107:XENON home page at Rice University
226:The detector was installed at the
33:research project, operated at the
14:
1539:Wolchover, Natalie (2020-06-17).
2865:
2854:
2853:
2261:
1849:"The Search for WIMPs Continues"
1793:Moskowitz, Clara (April 2021).
217:high-purity Germanium detectors
2821:Galaxy formation and evolution
2057:10.1103/PhysRevLett.100.021303
1999:10.1103/PhysRevLett.131.041002
1941:10.1103/PhysRevLett.131.041003
1883:10.1103/PhysRevLett.131.041002
1755:10.1103/PhysRevLett.129.161805
1375:10.1103/PhysRevLett.121.111302
1065:10.1103/PhysRevLett.111.021301
947:10.1103/physrevlett.109.181301
829:10.1103/PhysRevLett.101.091301
766:10.1103/PhysRevLett.100.021303
264:Gran Sasso National Laboratory
228:Gran Sasso National Laboratory
38:Gran Sasso National Laboratory
1:
536:10.1088/0954-3899/41/3/035201
165:minimal Supersymmetric models
163:available parameter space in
2243:Self-interacting dark matter
364:particles candidates called
16:Dark matter research project
2401:Navarro–Frenk–White profile
2391:Massive compact halo object
2386:Mass dimension one fermions
1847:Day, Charles (2023-07-28).
1664:10.1103/PhysRevD.104.063023
1564:Lin, Tongyan (2020-10-12).
1518:10.1103/PhysRevD.102.072004
1449:Moriyama, S. (2019-03-08).
2910:
1795:"Dark Matter's Last Stand"
1424:10.1038/d41586-019-01212-8
1183:10.1103/physrevd.83.082001
1128:10.1103/PhysRevD.90.062009
1010:10.1103/PhysRevD.84.061101
18:
2849:
2259:
2123:Dark matter limit plotter
2406:Scalar field dark matter
2248:Scalar field dark matter
2026:Physical Review Letters
1969:Physical Review Letters
1911:Physical Review Letters
1725:Physical Review Letters
1397:Suhonen, Jouni (2019).
1343:Physical Review Letters
1235:Physical Review Letters
1034:Physical Review Letters
916:Physical Review Letters
798:Physical Review Letters
735:Physical Review Letters
355:, a surprisingly large
332:double electron capture
94:time projection chamber
59:The experiment detects
54:time projection chamber
2271:Hypothetical particles
2253:Primordial black holes
2117:Katsuhi Arisaka, XENON
1591:10.1103/Physics.13.135
480:
427:
278:
211:
203:
147:
89:
21:Xenon (disambiguation)
2356:Dark globular cluster
2152:42.42056°N 13.51639°E
861:Astroparticle Physics
680:Astroparticle Physics
625:Astroparticle Physics
560:Astroparticle Physics
481:
428:
276:
209:
197:
152:Gran Sasso laboratory
144:
87:
2376:Dwarf galaxy problem
2298:Minicharged particle
2213:Baryonic dark matter
2087:The XENON Experiment
505:Journal of Physics G
441:
388:
19:For other uses, see
2148: /
2049:2008PhRvL.100b1303A
1991:2023PhRvL.131d1002A
1933:2023PhRvL.131d1003A
1875:2023PhRvL.131d1002A
1799:Scientific American
1747:2022PhRvL.129p1805A
1656:2021PhRvD.104f3023V
1582:2020PhyOJ..13..135L
1458:XENON collaboration
1415:2019Natur.568..462S
1366:2018PhRvL.121k1302A
1258:2017Natur.551..153G
1209:XENON collaboration
1175:2011PhRvD..83h2001A
1120:2014PhRvD..90f2009A
1057:2013PhRvL.111b1301A
1002:2011PhRvD..84f1101A
939:2012PhRvL.109r1301A
884:2011APh....35...43A
821:2008PhRvL.101i1301A
758:2008PhRvL.100b1303A
703:2011APh....34..679A
648:2014APh....54...11A
583:2012APh....35..573X
528:2014JPhG...41c5201A
294:for WIMP masses of
106:electroluminescence
74:Columbia University
2381:Halo mass function
2341:Cuspy halo problem
2157:42.42056; 13.51639
476:
423:
316:at a WIMP mass of
279:
212:
204:
148:
90:
80:Detector principle
2881:
2880:
2826:Illustris project
2760:
2759:
2233:Mixed dark matter
2228:Light dark matter
1633:Physical Review D
1409:(7753): 462–463.
1242:(7679): 153–154.
1152:Physical Review D
1097:Physical Review D
979:Physical Review D
221:mass spectrometry
219:. In a few cases
2901:
2869:
2868:
2857:
2856:
2421:
2361:Dark matter halo
2308:Sterile neutrino
2265:
2264:
2238:Warm dark matter
2218:Cold dark matter
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1818:Peres, Ricardo.
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1502:: 2006.09721v1.
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2841:UniverseMachine
2794:
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2735:
2653:
2647:
2425:
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2333:
2327:
2266:
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2223:Hot dark matter
2205:
2199:
2194:
2156:
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2017:Further reading
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1545:Quanta Magazine
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1483:. 28 July 2020.
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1267:10.1038/551153a
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592:10.1.1.255.9957
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357:magnetic moment
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126:fiducialization
98:photomultiplier
82:
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11:
5:
2907:
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2878:
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2875:
2863:
2850:
2847:
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2843:
2838:
2833:
2831:Imaginary mass
2828:
2823:
2818:
2813:
2808:
2802:
2800:
2796:
2795:
2793:
2792:
2787:
2782:
2780:HVC 127-41-330
2777:
2771:
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2762:
2761:
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2740:Other projects
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2366:Dark radiation
2363:
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2343:
2337:
2335:
2329:
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2326:
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2094:
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2081:External links
2079:
2078:
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2018:
2015:
2013:
2012:
1954:
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1810:
1785:
1760:
1731:(16): 161805.
1714:
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1622:
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1556:
1531:
1486:
1469:
1438:
1389:
1350:(11): 111302.
1328:
1303:
1292:. May 24, 2017
1281:
1220:
1196:
1141:
1086:
1023:
968:
923:(18): 181301.
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687:(9): 679–698.
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2816:Exotic matter
2814:
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2785:Smith's Cloud
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2767:dark galaxies
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2033:(2): 021303.
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2020:
2016:
2008:
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2000:
1996:
1992:
1988:
1983:
1978:
1975:(4): 041002.
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1917:(4): 041003.
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1610:Physics World
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1316:UChicago News
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1159:(8): 082001.
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1129:
1125:
1121:
1117:
1112:
1107:
1104:(6): 062009.
1103:
1099:
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1087:
1082:
1078:
1074:
1070:
1066:
1062:
1058:
1054:
1049:
1044:
1041:(2): 021301.
1040:
1036:
1035:
1027:
1024:
1019:
1015:
1011:
1007:
1003:
999:
994:
989:
986:(6): 061101.
985:
981:
980:
972:
969:
964:
960:
956:
952:
948:
944:
940:
936:
931:
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922:
918:
917:
909:
906:
901:
897:
893:
889:
885:
881:
876:
871:
867:
863:
862:
854:
851:
846:
842:
838:
834:
830:
826:
822:
818:
813:
808:
805:(9): 091301.
804:
800:
799:
791:
788:
783:
779:
775:
771:
767:
763:
759:
755:
750:
745:
742:(2): 021303.
741:
737:
736:
728:
725:
720:
716:
712:
708:
704:
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695:
690:
686:
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541:
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512:(3): 035201.
511:
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498:
495:
489:
487:
471:
467:
463:
458:
455:
451:
447:
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435:LZ experiment
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114:scintillation
110:
107:
103:
102:scintillation
99:
95:
86:
79:
77:
75:
71:
66:
62:
61:scintillation
57:
55:
51:
47:
43:
39:
36:
32:
29:
22:
2870:
2858:
2632:
2133:
2030:
2024:
1972:
1968:
1957:
1914:
1910:
1899:
1856:
1852:
1842:
1830:. Retrieved
1826:
1813:
1802:. Retrieved
1798:
1788:
1777:. Retrieved
1772:
1763:
1728:
1724:
1717:
1706:. Retrieved
1704:. 2022-07-22
1702:Science News
1701:
1692:
1680:
1637:
1631:
1625:
1614:. Retrieved
1612:. 2020-10-15
1609:
1600:
1573:
1569:
1559:
1548:. Retrieved
1544:
1534:
1499:
1496:Phys. Rev. D
1495:
1489:
1461:. Retrieved
1457:
1406:
1402:
1392:
1347:
1341:
1331:
1320:. Retrieved
1318:. 2017-05-18
1315:
1306:
1294:. Retrieved
1284:
1239:
1233:
1223:
1212:. Retrieved
1208:
1199:
1156:
1150:
1144:
1101:
1095:
1089:
1038:
1032:
1026:
983:
977:
971:
920:
914:
908:
868:(2): 43–49.
865:
859:
853:
802:
796:
790:
739:
733:
727:
684:
678:
672:
629:
623:
617:
564:
558:
552:
509:
503:
497:
383:
379:
375:
349:
345:
325:
319:
318:30 GeV/
307:
297:
296:35 GeV/
280:
269:
261:
253:
242:
241:65 GeV/
225:
213:
184:
178:
177:30 GeV/
161:
149:
131:
122:
111:
91:
70:Elena Aprile
58:
27:
25:
2811:Dark energy
2775:HE0450-2958
2417:experiments
2351:Dark galaxy
2334:and objects
2288:Dark photon
2206:dark matter
2197:Dark matter
2155: /
1859:(4): s106.
1775:(in French)
362:dark energy
182:WIMP mass.
42:dark matter
31:dark matter
2806:Antimatter
2765:Potential
2493:DAMA/LIBRA
2346:Dark fluid
2303:Neutralino
2143:13°30′59″E
2140:42°25′14″N
1982:2207.03764
1924:2303.14729
1866:2207.03764
1804:2021-04-13
1779:2020-06-30
1738:2207.11330
1708:2022-08-03
1647:2103.15834
1616:2020-10-23
1550:2020-06-18
1509:2006.09721
1463:2020-11-18
1357:1805.12562
1322:2017-05-29
1249:1705.06655
1214:2017-06-02
490:References
366:chameleons
314:10 cm
292:10 cm
237:10 cm
173:10 cm
118:ionization
65:ionization
2790:VIRGOHI21
2747:MultiDark
2654:detection
2538:EDELWEISS
2426:detection
2371:Dark star
2040:0706.0039
1672:232417159
1526:222338600
1166:1101.3866
1111:1404.1455
1048:1301.6620
1018:118604915
993:1104.3121
930:1207.5988
900:119223885
875:1103.5831
812:0805.2939
749:0706.0039
719:118661045
694:1001.2834
639:1207.3458
632:: 11–24.
587:CiteSeerX
574:1107.2155
519:1311.1088
456:−
448:×
403:−
395:×
2888:Category
2860:Category
2652:Indirect
2508:DarkSide
2498:DAMA/NaI
2332:Theories
2204:Forms of
2065:18232850
2007:37566836
1949:37566859
1891:37566836
1832:22 March
1433:31019322
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