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[Significance] Numerous astronomical observations have confirmed the existence of dark matter in the universe. Weakly Interacting Massive Particles(WIMPs) can naturally form in the early universe, and if they exist stably, their mass density satisfies the constraints imposed by astronomical observations. These properties make WIMPs one of the most promising candidates for dark matter. Their detection methods include direct detection, indirect detection, and collider detection, often described as the approaches of “reaching for the sky, delving into the earth, and venturing to the Antarctic.” Xenon, an inert element, has become an optimal target material for the direct detection of WIMP dark matter particles owing to its unique physical and chemical properties. Internationally, major detection experiments using liquid xenon as the target material include XENON, LUX-ZEPLIN(LZ), and PandaX, and the dual-phase time projection chamber(DPTPC) is the core technology for dark matter detection. As one of the most cutting-edge scientific directions of the 21 st century, dark matter research may hold the key to revealing the fundamental laws of the universe. By elaborating on a series of achievements in the field of dark matter research, this paper enables readers to understand international experimental technologies and scientific progress in liquid xenon–based dark matter detection. [Progress] XENON10 was the world's first liquid xenon–based dark matter detection experiment, which sets a limit of 8.8 × 10-44 cm2 for WIMPs with a mass of 100 GeV/c2. XENON100 increased the target mass to 10 times that of XENON10, allowing it to place a stringent limit of 2.0 × 10-45 cm2 on the spin-independent nucleon scattering of WIMPs with a mass of 55 GeV/c2. With a target mass 32 times that of XENON100, XENON1T sets a cross-section limit of 1.6 × 10-47 cm2 for spin-independent WIMP–nucleon scattering at a mass of 50 GeV/c2. XENONnT is a rapid upgrade based on XENON1T; using 97.1 days of valid data, it reported a minimum upper cross-section limit of 2.58 × 10-47 cm2 for spin-independent WIMP–nucleon scattering at a mass of 28 GeV/c2. Using 85.3 days of scientific data, LUX sets a minimum upper cross-section limit of 7.6 × 10-46 cm2 for spin-independent WIMP–nucleon scattering at a mass of 33 GeV/c2. An analysis of its complete 95-day dataset yielded a minimum upper cross-section limit of 6.0 × 10-46 cm2 at the same mass. Based on 332 days of newly acquired data, LUX sets an upper exclusion limit of 2.2 × 10-46 cm2 for spin-independent WIMP interactions at a mass of 50 GeV/c2. A combined analysis of two LUX phases excluded a minimum cross-section of 1.1 × 10-46 cm2 for WIMPs at 50 GeV/c2 and set a minimum upper cross-section limit of 1.6 × 10-41 cm2 for spin-dependent WIMP–nucleon scattering at a mass of 35 GeV/c2. The ZEPLIN-III detector, using 319 days of data, excluded a cross-section limit of 4.8 × 10-44 cm2 for WIMPs with a mass near 50 GeV/c2. LZ, an upgraded experiment building on the foundations of LUX and ZEPLIN-III, used 60 days of valid data collected between 2021 and 2022 to set a cross-section limit of 9.2 × 10-48 cm2 for spin-independent WIMP–nucleon scattering at a mass of 36 GeV/c2. By combining 220 days of data collected between 2023 and 2024 with the previous 60-day dataset, LZ placed world-leading limits on spin-independent and spin-dependent WIMP–nucleon scattering interactions for WIMP masses ≥9 GeV/c2. [Conclusions and Prospects] To achieve more precise detection of dark matter signals, the XLZD collaboration has been established by the XENON, LZ, and DARWIN experiments, with the goal of constructing and operating a next-generation dark matter detector. The XLZD detector will exceed the scale of DARWIN and further close the gap to the “ neutrino fog.” With the completion of the next-generation dark matter detector by 2030, XLZD may enable the discovery of dark matter particles in the universe. This breakthrough would help humanity solve a puzzle that has persisted for nearly a century and open new avenues for understanding the universe.
[1]ZWICKY F. Die Rotverschiebung von extragalaktischen Nebeln[J]. Helvetica Physica Acta, 1933, 6:110–127.
[2]苏萌.暗物质的天文学探测[J].科技导报, 2016, 34(5):14–21.SU M. Astronomical approach of dark matter detection[J].Science&Technology Review, 2016, 34(5):14–21.(in Chinese)
[3]黄晓渊.暗物质间接探测研究进展[J].中国科学:物理学力学天文学, 2025, 55(1):156–167.HUANG X Y. Progress in the dark matter indirect detection[J].Scientia Sinica(Physica, Mechanica&Astronomica), 2025,55(1):156–167.(in Chinese)
[4]舒以科,尹纪龙,王毅,等.在零下186℃液氩中探索暗物质奥秘[J].中国科学:物理学力学天文学, 2025, 55(11):111003.SHU Y K, YIN J L, WANG Y, et al. Exploring the mysteries of dark matter with liquidargon at–186℃[J]. Scientia Sinica(Physica, Mechanica&Astronomica), 2025, 55(11):111003.(in Chinese)
[5]季向东,张新民,谌勋.中国暗物质与暗能量研究5~10年展望[J].科学通报, 2016, 61(11):1181–1187.JI X D, ZHANG X M, CHEN X. A road-map for dark matter and dark energy research in China[J]. Chinese Science Bulletin,2016, 61(11):1181–1187.(in Chinese)
[6]DE LOS HEROS C P. Status, challenges and directions in indirect dark matter searches[J]. Symmetry-Basel, 2020, 12(10):1648.
[7]MISIASZEK M, ROSSI N. Direct detection of dark matter:A critical review[J]. Symmetry-Basel, 2024, 16(2):201.
[8]BOVEOA A, DOGLIONI C. Dark matter searches at colliders[J].Annual Review of Nuclear and Particle Science, 2018, 68:429–459.
[9]BAUDIS L. WIMP dark matter direct-detection searches in noble gases[J]. Physics of the Dark Universe, 2014, 4:50–59.
[10]APRILE E, AALBERS J, ABE K, et al. The XENONnT dark matter experiment[J]. European Physical Journal C, 2024,84(8):784.
[11]AALBERS J, AKERIB D S, AKERLOF C W, et al. First dark matter search results from the LUX-ZEPLIN(LZ)experiment[J].Physical Review Letters, 2023, 131(4):041002.
[12]ZHANG H G, ABDUKERIM A, CHEN W, et al. Dark matter direct search sensitivity of the PandaX-4T experiment[J].Science China-Physics Mechanics&Astronomy, 2019, 62(3):31011.
[13]BARNABA O, CHEN Y B, MUSITELLI G, et al. A fullintegrated pulse-shape discriminator for liquid scintillator counters[J]. Nuclear Instruments&Methods in Physics Research Section A-Accelerators Spectrometers Detectors and Associated Equipment, 1998, 410:220-228.
[14]APRILE E, ARISAKA K, ARNEODO F. First dark matter results from the XENON100 experiment[J]. Physical Review Letters, 2010, 105(13):131302.
[15]ALNER G J, ARAUJO H M, BEWICK A, et al. First limits on WIMP nuclear recoil signals in ZEPLIN-II:A two phase xenon detector for dark matter detection[J]. Astroparticle Physics,2007, 28(3):287–302.
[16]LEBEDENKO V N, ARAUJO H M, BARNES E J, et al. Limits on the spin-dependent WIMP-nucleon cross sections from the first science run of the ZEPLIN-III experiment[J]. Physical Review Letters, 2009, 103(15):151302.
[17]ANGLE J, APRILE E, ARNEODO F, et al. First results from the XENON10 dark matter experiment at the gran sasso national laboratory[J]. Physical Review Letters, 2008, 100(2):021303.
[18]APRILE E, ARISAKA K, ARNEODO F, et al. The XENON100dark matter experiment[J]. Astroparticle Physics, 2012, 35(9):573–590.
[19]APRILE E, ALFONSI M, ARIISAKA K, et al. Dark matter results from 225 live days of Xenon100 data[J]. Physical Review Letters, 2012, 109(18):181301.
[20]APRILE E, AALBERS J, AGOSTINI F, et al. Physics reach of the XENON1T dark matter experiment[J]. Journal of Cosmology and Astroparticle Physics, 2016, 4:027.
[21]APRILE E, AALBERS J, AGOSTINI F, et al. The XENON1T dark matter experiment[J]. European Physical Journal C, 2017,77(12):881.
[22]APRILE E, AALBERS J, AGOSTINI F, et al. First dark matter search results from the XENON1T experiment[J]. Physical Review Letters, 2017, 119(18):181301.
[23]APRILE E, AALBERS J, AGOSTINI F, et al. Projected WIMP sensitivity of the XENONnT dark matter experiment[J]. Journal of Cosmology and Astroparticle Physics, 2020, 11:031.
[24]MANALAYSAY A, UNDAGOITIA T M, ASKIN A, et al.spatially uniform calibration of a liquid xenon detector at low energies using 83 mKr[J]. Review of Scientific Instruments,2010, 81(7):073303.
[25]LANG R F, BROWN A, BROWN E, et al. A 220Rn source for the calibration of low-background experiments[J]. Journal of Instrumentation, 2016, 11:P04004.
[26]APRILE E, ABE K, AGOSTINI F, et al. Low-energy calibration of XENON1T with an internal 37Ar source[J]. European Physical Journal C, 2023, 83(6):542.
[27]APRILE E, AALBERS J, ABE K, et al. The triggerless data acquisition system of the XENONnT experiment[J]. Journal of Instrumentation, 2023, 18(7):P07054.
[28]AALBERS J, ANGEVAARE J R, WENZ D, et al. AxFoundation/strax:v1.6.4.Zenodo, 2024[EB/OL]. https:zenodo.org/records/11355772.
[29]ANGEVAARE J R, AALBERS J, WENZ D, et al. XENONnT/straxen:v2.2.6.Zenodo, 2024[EB/OL]. https://zenodo.org/records/13902448.
[30]刘可欣,徐大成,高飞. XENON暗物质和中微子实验[J].中国科学:物理学力学天文学, 2025, 55(11):111004.LU K X, XU D C, GAO F. The XENON dark matter and neutrino experiment[J]. Scientia Sinica(Physica, Mechanica&Astronomica), 2025, 55(11):111004.(in Chinese)
[31]APRILE E, ABE K, AGOSTINI F, et al. First dark matter search with nuclear recoils from the XENONnT experiment[J].Physical Review Letters, 2023, 131(4):041003.
[32]AKERIB D S, BAI X, BEDIKIAN S, et al. The large underground xenon(LUX)experiment[J]. Nuclear Instruments&Methods in Physics Research Section A-Accelerators Spectrometers Detectors and Associated Equipment, 2013, 704:111–126.
[33]BOLOZDYNYA A, BRADLEY A, BRYAN S, et al. Cryogenics for the LUX detector[J]. IEEE Transactions on Nuclear Science,2009, 56(4):2309–2312.
[34]KASTENS L W, CAHN S B, MANZUR A, et al. Calibration of a liquid xenon detector with 83Krm[J]. Physical Review C, 2009,80(4):045809.
[35]AKERIB D S, BAI X, BERNARD E, et al. An ultra-low background PMT for liquid xenon detectors[J]. Nuclear Instruments&Methods in Physics Research Section AAccelerators Spectrometers Detectors and Associated Equipment,2013, 703:1–6.
[36]AKERIB D S, BAI X, BEDIKIAN S, et al. Data acquisition and readout system for the LUX dark matter experiment[J]. Nuclear Instruments&Methods in Physics Research Section A-Accelerators Spectrometers Detectors and Associated Equipment, 2012, 668:1–8.
[37]AKERIB D S, ARAUJO H M, BAI X, et al. First result from the LUX dark matter experiment at the Sanford underground research facility[J]. Physical Review Letters, 2014, 112(9):091303.
[38]PASCOAL DA SILVA C F. Dark matter searches with LUX[Z].arXiv:1710.03572v1[hep-ex], 2017.
[39]AKERIB D S, ALSUM S, ARAUJO H M, et al. Results from a search for dark matter in the complete LUX exposure[J].Physical Review Letters, 2017, 118(2):021303.
[40]AKERIB D S, ALSUM S, ARAUJO H M, et al. Limits on spin-dependent WIMP-nucleon cross section obtained from the complete LUX exposure[J]. Physical Review Letters, 2017,118(25):251.
[41]ALNER G J, ATAC M, BEWICK A, et al. Status of the ZEPLIN II experiment[J]. New Astronomy Reviews, 2005, 49(2-6):259–263.
[42]LEBEDENKO V N, ARAUJO H M, BARNES E J, et al. Results from the first science run of the ZEPLIN-III dark matter search experiment[J]. Physical Review D, 2009, 80(5):052010.
[43]AKIMOV D Y, ARAUJO H M, BARNES E J, et al. WIMPnucleon cross-section results from the second science run of ZEPLIN-III[J].Physics Letters B, 2012, 709(1-2):14–20.
[44]AKERIB D S, AKERLOF C W, ALSUM S K, et al. Projected WIMP sensitivity of the LUX-ZEPLIN(LZ)dark matter experiment[J]. Physical Review D, 2020, 101(5):052002.
[45]AKERIB D S, AKERLOF C W, AKIMOV D Y, et al.Identification of radiopure titanium for the LZ dark matter experiment and future rare event searches[J]. Astroparticle Physics, 2017, 96:1–10.
[46]AKERIB D S, AKERLOF C W, AKIMOV D Y, et al. The LUX-ZEPLIN(LZ)experiment[J]. Nuclear Instruments&Methods in Physics Research Section A-Accelerators Spectrometers Detectors and Associated Equipment, 2020, 953:163047.
[47]AKERIB D S, AKERLOF C W, ALQAHTANI A, et al.Simulations of events for the LUX-ZEPLIN(LZ)dark matter experiment[J]. Astroparticle Physics, 2021, 125:102480.
[48]AALBERS J, AKERIB D S, AL MUSALHI A K, et al.Background determination for the LUX-ZEPLIN(LZ)dark matter experiment[J]. Physical Review D, 2023, 108(1):012010.
[49]AALBERS J, AKERIB D S, AL MUSALHI A K, et al. Dark matter search results from 4.2 tonne-years of exposure of the LUX-ZEPLIN(LZ)experiment[J]. Physical Review Letters,2025, 135(1):011802.
[50]BAUDIS L. DARWIN/XLZD:A future xenon observatory for dark matter and other rare interactions[J]. Nuclear Physics B,2024, 1003:116473.
Basic Information:
DOI：10.16791/j.cnki.sjg.2026.01.008
China Classification Code:P145.9
Citation Information:
[1]SHAO Pengfei.Experimental technologies and scientific achievements of international liquid xenon-based dark matter detection[J].Experimental Technology and Management,2026,43(01):58-65.DOI:10.16791/j.cnki.sjg.2026.01.008.