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The XENONnT Dark Matter Experiment

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arxiv 2402.10446 v2 pith:TS7E6AUL submitted 2024-02-16 physics.ins-det astro-ph.IMhep-ex

XENON Collaboration: E. Aprile , J. Aalbers , K. Abe , S. Ahmed Maouloud , L. Althueser , B. Andrieu , E. Angelino , J. R. Angevaare
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V.C. Antochi D. Antón Martin F. Arneodo M. Balata L. Baudis A. L. Baxter M. Bazyk L. Bellagamba R. Biondi A. Bismark E. J. Brookes A. Brown S. Bruenner G. Bruno R. Budnik T. K. Bui C. Cai J. M. R. Cardoso F. Cassese A. Chiarini D. Cichon A. P. Cimental Chavez A. P. Colijn J. Conrad R. Corrieri J. J. Cuenca-García J. P. Cussonneau O. Dadoun V. D'Andrea M. P. Decowski B. De Fazio P. Di Gangi S. Diglio J. M. Disdier D. Douillet K. Eitel A. Elykov S. Farrell A. D. Ferella C. Ferrari H. Fischer M. Flierman S. Form D. Front W. Fulgione C. Fuselli P. Gaemers R. Gaior A. Gallo Rosso M. Galloway F. Gao R. Gardner N. Garroum R. Glade-Beucke L. Grandi J. Grigat H. Guan M. Guerzoni M. Guida R. Hammann A. Higuera C. Hils L. Hoetzsch N. F. Hood J. Howlett C. Huhmann M. Iacovacci G. Iaquaniello L. Iven Y. Itow J. Jakob F. Joerg A. Joy M. Kara P. Kavrigin S. Kazama M. Kobayashi G. Koltman A. Kopec F. Kuger H. Landsman R. F. Lang L. Levinson I. Li S. Li S. Liang S. Lindemann M. Lindner K. Liu J. Loizeau F. Lombardi J. Long J. A. M. Lopes Y. Ma C. Macolino J. Mahlstedt A. Mancuso L. Manenti F. Marignetti T. Marrodán Undagoitia P. Martella K. Martens J. Masbou D. Masson E. Masson S. Mastroianni E. Mele M. Messina R. Michinelli K. Miuchi A. Molinario S. Moriyama K. Mor{aa} Y. Mosbacher M. Murra J. Müller K. Ni S. Nisi U. Oberlack D. Orlandi R. Othegraven B. Paetsch J. Palacio S. Parlati P. Paschos Q. Pellegrini R. Peres C. Peters J. Pienaar M. Pierre G. Plante T. R. Pollmann J. Qi J. Qin D. Ramírez García M. Rynge J. Shi R. Singh L. Sanchez J. M. F. dos Santos I. Sarnoff G. Sartorelli J. Schreiner D. Schulte P. Schulte H. Schulze Ei{ss}ing M. Schumann L. Scotto Lavina M. Selvi F. Semeria P. Shagin S. Shi E. Shockley M. Silva H. Simgen J. Stephen M. Stern B. K. Stillwell A. Takeda P.-L. Tan D. Tatananni A. Terliuk D. Thers F. Toschi G. Trinchero C. Tunnell F. Tönnies K. Valerius G. Volta C. Weinheimer M. Weiss D. Wenz J. Westermann C. Wittweg T. Wolf V. H. S. Wu Y. Xing D. Xu Z. Xu M. Yamashita L. Yang J. Ye L. Yuan G. Zavattini M. Zhong T. Zhu
This is my paper · ORCID
classification physics.ins-detastro-ph.IMhep-ex
keywords experimentdarkmatterxenonxenonntactivedetectorliquid
verification ladder T0 review T1 audit T2 compute T3 formal
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The multi-staged XENON program at INFN Laboratori Nazionali del Gran Sasso aims to detect dark matter with two-phase liquid xenon time projection chambers of increasing size and sensitivity. The XENONnT experiment is the latest detector in the program, planned to be an upgrade of its predecessor XENON1T. It features an active target of 5.9 tonnes of cryogenic liquid xenon (8.5 tonnes total mass in cryostat). The experiment is expected to extend the sensitivity to WIMP dark matter by more than an order of magnitude compared to XENON1T, thanks to the larger active mass and the significantly reduced background, improved by novel systems such as a radon removal plant and a neutron veto. This article describes the XENONnT experiment and its sub-systems in detail and reports on the detector performance during the first science run.

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Forward citations

Cited by 8 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Light Dark Matter Search with 7.8 Tonne-Year of Ionization-Only Data in XENONnT

    hep-ex 2026-01 conditional novelty 6.0 of 10

    An S2-only analysis of 7.83 tonne-years of XENONnT data finds no dark matter excess and sets 90% CL limits, e.g. 6.0e-45 cm^2 for spin-independent scattering at 5 GeV/c^2.

  2. Design of a Large Area Digital SiPM with High Fill Factor and Fully Serial Digital Readout for Single Photon Detection in Liquid Noble Gas Detectors

    physics.ins-det 2025-01 conditional novelty 6.0 of 10

    A large-area digital SiPM with 72.5% fill factor reads individual photon hits with 10 ns timing through a four-signal serial interface.

  3. A Novel Low-Background Photomultiplier Tube Developed for Xenon Based Detectors

    physics.ins-det 2024-12 conditional novelty 6.0 of 10

    The R12699 PMT reaches ~0.08 mBq/PMT 60Co and ~0.06 mBq/PMT 238U late chain radioactivity, 15-fold lower than PandaX-4T's R11410, with cryogenic gain of 4.23e6 and 2.5 Hz dark count rate.

  4. MOTION, a liquid xenon time projection chamber platform for high voltage technologies in dark matter detectors

    physics.ins-det 2026-08 conditional novelty 5.0 of 10

    A new 70 kg liquid xenon test stand, MOTION, is constructed and commissioned for studying high-voltage breakdown and electrode surfaces, but its 200 kV physics program is still planned.

  5. Direct detection of solar chameleons with electron recoil data from XENONnT

    hep-ph 2025-11 conditional novelty 5.0 of 10

    XENONnT electron-recoil data bound solar chameleons to log10 β_eff < −6.9, independent of the potential index n for inverse power-law chameleons at the dark-energy scale.

  6. Performance of FBK VUV-HD3 and HPK VUV4 SiPMs in the Light-only Liquid Xenon (LoLX) Detector

    physics.ins-det 2025-10 unverdicted novelty 5.0 of 10

    In-situ comparison in liquid xenon finds HPK VUV4 SiPMs detect 33–38% less scintillation light than FBK VUV-HD3 SiPMs, attributed to surface shadowing at oblique photon incidence.

  7. Radon Removal in XENONnT down to the Solar Neutrino Level

    physics.ins-det 2025-02 conditional novelty 5.0 of 10

    XENONnT reduced radon-222 in its liquid xenon target to 0.90 ± 0.07 micro-becquerel per kilogram, the lowest level reported for an operational dual-phase dark matter detector, matching the solar neutrino background.

  8. Dark Matter Freeze-In during Warm Inflation and the Seesaw Mechanism

    hep-ph 2024-12 conditional novelty 4.0 of 10

    A U(1)_{B-L} inverse-seesaw model realizes warm-inflation freeze-in of fermionic dark matter via a heavy Z' portal, with parameters adjusted to match the observed dark matter abundance and neutrino masses.

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