The XLZD Design Book: towards the next-generation liquid xenon observatory for dark matter and neutrino physics

Abstract This report describes the experimental strategy and technologies for XLZD, the next-generation xenon observatory sensitive to dark matter and neutrino physics. In the baseline design, the detector will have an active liquid xenon target of 60 tonnes, which could be increased to 80 tonnes if the market conditions for xenon are favorable. It is based on the mature liquid xenon time projection chamber technology used in current-generation experiments, LZ and XENONnT. The report discusses the baseline design and opportunities for further optimization of the individual detector components. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3 $$\sigma $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>σ</mml:mi> </mml:math> evidence potential for WIMP-nucleon cross sections as low as $$3\times 10^{-49}\mathrm \,cm^2$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mn>3</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>49</mml:mn> </mml:mrow> </mml:msup> <mml:mspace/> <mml:mi>c</mml:mi> <mml:msup> <mml:mi>m</mml:mi> <mml:mn>2</mml:mn> </mml:msup> </mml:mrow> </mml:math> (at 40 GeV/c $$^2$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mmultiscripts> <mml:mrow/> <mml:mrow/> <mml:mn>2</mml:mn> </mml:mmultiscripts> </mml:math> WIMP mass). The observatory will also have leading sensitivity to a wide range of alternative dark matter models. It is projected to have a 3 $$\sigma $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>σ</mml:mi> </mml:math> observation potential of neutrinoless double beta decay of $$^{136}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mmultiscripts> <mml:mrow/> <mml:mrow/> <mml:mn>136</mml:mn> </mml:mmultiscripts> </mml:math> Xe at a half-life of up to $$5.7\times 10^{27}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mn>5.7</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>27</mml:mn> </mml:msup> </mml:mrow> </mml:math> years. Additionally, it is sensitive to astrophysical neutrinos from the sun and galactic supernovae.

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Journal
The European Physical Journal C
Published
2025-10-23
DOI
https://doi.org/10.1140/epjc/s10052-025-14810-w
Citations
7
Primary Topic
Dark Matter and Cosmic Phenomena
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article
Field-Weighted Citation Impact
13.09

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article

The XLZD Design Book: towards the next-generation liquid xenon observatory for dark matter and neutrino physics

M. Kara, J. W. Bargemann, M. Yeh, K. J. Palladino et al.
7 citations
The European Physical Journal C
Dark Matter and Cosmic Phenomena
13.09
article

The XLZD Design Book: towards the next-generation liquid xenon observatory for dark matter and neutrino physics

M. Kara, J. W. Bargemann, M. Yeh, K. J. Palladino, F. Lombardi, Nicole F. Bell, R. L. Kirk, K. Martens, V. H. S. Wu, F Kahlert, G. Zavattini, C. Hils, L. J. Levinson, P. Di Gangi, G. Trinchero, J E Armstrong, S. Moriyama, S. Lindemann, D. Q. Huang, E. Hartigan-O’Connor, A. K. Al Musalhi, M. Babicz, B. Antunović, P. Kavrigin, W. Zha, L. Kreczko, J. Lin, Y. Itow, C. Wittweg, S. Y. Shi, G.J. Davies, R. Gibbons, C. Di Donato, F. Alder, H. J. Birch, K. Eitel, Donald F. Hunt, S. Shaw, V. N. Solovov, F. Gao, Veronica Mazza, S. Wüstling, R. Budnik, H. Simgen, E. D. Fraser, V. Hannen, G. Pereira, G. Plante, J. Grigat, R. L. Mannino, A. Li, J. Schreiner, T Stenhouse, J. Qin, Κ. Zuber, Jing Xu, H. Chen, M. Yamashita, M. Arthurs, N. Garroum, E. Mizrachi, C. Capelli, R. J. Gaitskell, V. Velan, Aya Takeda, E. Masson, T. P. Biesiadzinski, E. Morrison, Joseph McLaughlin, Peter Schulte, B. J. Mount, M. Steidl, J. J. Cuenca-García, M. Pierre, D. Khaitan, A. Stevens, E. H. Miller, E. Jacquet, Z. Tong, L. Althueser, Jayden L. Newstead, C. Fuselli, L. Baudis, K. Liu, D. S. Leonard, Y. Mosbacher, D. N. McKinsey, V. Kudryavtsev, M Obradović, David Woodward, L. J. Cooper, N. Fieldhouse, G. Sinev, D. Vorkapic, S. A. Hertel, A. Kopec, John M. DelGaudio, M. Flierman, D Wenz, M Doerenkamp, M.A. Hernández, Timothy J. Hall, D. Kodroff, D. Santone, M. Murdy, C. Hall, M. Tripathi, S. Woodford, A. Bismark, A. Elykov, M. Galloway, F. Glück, Erin Bishop, Y. Biondi, W. Fulgione, J. Loizeau, E. Aprile, A. D. Ferella, H. U. Flaecher, M. Wurm, A. Basharina-Freshville, J. E. Y. Dobson, C. McCabe, L. Hoetzsch, E. Druszkiewicz, J. O’Dell, J. J. Haiston, F. L. H. Wolfs, L Manenti, M. Iacovacci, K. Morå, D. S. Akerib, W. C. Taylor, A. Cottle, M. Guida, C. Lu, C. A. Rhyne, M. C. Carmona-Benitez, R Giacomobono, M. Trask, S. D. Jones, R. W. Schnee, Jing-Zhao Qi, N. Kurita, Roberto Trotta, I. Olcina, Ruben Coronel, C. Weinheimer, K. Wild, L. de Viveiros, P Kharbanda, M. P. Decowski, A. Razeto, Gianluca Lucchetti, R. S. James, Alexander A. Baker, P. Urquijo, Marius Keller, P. Sánchez-Lucas, I. Lopes, R. Glade-Beucke, M. Williams, D. Rynders, G. Drexlin, S. Brommer, Y. Xing, Q. Xia, R. Rosero, Sara K. Lindén, Martin Hoferichter, A. Higuera, F. Pompa, S. Mastroianni, J. Palmer, Chris J. Wright, A. Deisting, Markus Klute, S. Kazama, K. T. Lesko, J. Wolf, S. Ahmed Maouloud, D. Ramírez García, J. Aalbers, H. S. Riyat, Robin Größle, Rie Miyata, F. Neves, Lili Yang, M. Selvi, J. J. Wang, A. Kamaha, S. Vecchi, C. Silva, R. F. Lang, J. Tranter, J. Genovesi, G. R. C. Rischbieter, Andre Scaffidi, Kenzo Hiraoka, S. Li, K. Ni, T. Pershing, D. Thers, Kenneth Clark, V. D’Andrea, N. F. Hood, J. Masbou, M. Bazyk, Y Kaminaga, K. Boese, M. V. Converse, J.M.F. dos Santos, M Loutit, G. D. Orebi Gann, K. Beattie, P. Kemp-Russell, A. Piepke, B. Penning, T. Fruth, C. S. Amarasinghe, K. M. Weerman, F. Piastra, T. Marrodán Undagoitia, A. B. M. R. Sazzad, A. C. Vaitkus, Róbert Braun, R. Biondi, T. Rushton, H. M. Araújo, S. Milutinovic, B. Paetsch, T. R. Pollmann, A. Brown, C. M. B. Monteiro, H. Nelson, N. M. Fearon, E. Morteau, A. Schwenk, T.M. Benson, A. Geffre, M. Schümann, Adrian Schwenck, J. A. M. Lopes, M. E. Monzani, T. Shimada, K. C. Oliver-Mallory, T.C. Luce, P. Brás, S. J. Haselschwardt, D. Bauer, B. von Krosigk, M. Lindner, A. Manalaysay, F. Tönnies, E. Perry, Y. Wang, Louis A. Sherman, A. Lindote, C. Maupin, C. Tunnell, M. Horn, S. Burdin, A. Chawla, Céline Bœhm, C. Cai, Kazuo Fujikawa, T. J. Whitis, M. Pandurović, D. J. Taylor, B. Lehnert, A. St. J. Murphy, P. Gaemers, S. R. Eriksen, Sandeep S. Davé, R. Saakyan, D. W. P. Amaral, A. P. Cimental Chávez, Miquel Adrover, Zaiwei Song, U. Oberlack, L. Grandi, C. Ghag, R. Peres, T. J. Sumner, W. Lorenzon, W. H. Lippincott, A. Ames, L Principe, N Hargittai, N. J. Pannifer, G. J. Homenides, M Rajado, T Flehmke, A Melchiorre, E. E. Barillier, J. Siniscalco, O. Valentino, L. Di Felice, Bo Yu, G. Bella, Zhiying Li, Ding Chen, Michael Carter, Ailing Wang, Jonathan Green, A. Roy, S. T. Wilson, S. Ghosh, A. Bhatti, M. Messina, R. Singh, Wei Shen, Y. Xu, Ke Qiao, J. Menéndez, K. Abe, H. Fischer, P.-L. Tan, Matthew J. Weiss, N. Gallice, Jan Conrad, A. Mancuso, J. Soria, Matthew Stanley, F. Toschi, Sourav Dey, C. Macolino, J. Pienaar, M. McCarthy, H. Landsman, Dong Xu, D. Waters, D. Cussans, M. Kleifges, N. Chott, A. Nguyen, K. Y. Oyulmaz, B. Kilminster, D Koke, J. Patton, L. C. Daniel Garcia, R. Hammann, I. Li, H. Schulze Eißing, J. Jakob, M. Zhong, F. Semeria, E. Barberio, J. Mahlstedt, G. Volta, L. Scotto Lavina, F. Girard, Simon Fayer, G. Sartorelli, D. Costanzo, A. Naylor, A. David, P. Shagin, J. J. Cherwinka, A. P. Colijn, B. Maier, H. Kraus, E. V. Korolkova, S. Diglio, M. G. Wilson, S. Hansmann-Menzemer, V. Radeka, M. Murra, S. Kravitz, K. Stifter, Junho Kim, Jiri Müller, J. Lee, C O'Hare, J. J. Silk, P. Sorensen, J. Orpwood, D. R. Tovey, D. R. Tronstad, M. Worcester, R. Engel, G. Bruni, F Marignetti, C. Brew, Q. Pellegrini, K Valerius, P. A. Majewski, G. Carini, S. Paramesvaran, J. Reichenbacher, F. Kuger, R. Gaïor, D. R. Tiedt, T. Shutt, M. Solmaz, E. Angelino, Tom Marley, A. Breskin, G. A. Cox, M. G. D. van der Grinten, A. Richards, N. Beaupère, Y. T. Chin, A. Chauvin, K. Miuchi, S. Gokhale, N. Angelides, J. Bang, Shaun M. G. Hughes, D. Curran, D. Colling, S. Luitz, A. Molinario, A. E. Bolotnikov, T. Thümmler, L. Escudero Sanchez, F. Joerg, A. C. Kaboth, A. Ravindran, A. Usón, Ye J, M. Utoyama, M. Balzer, Y. Qie, H. Guan, B Milosovic, S Ouahada, C. L. Dunbar, C. Lawes, S. Radeka, I. Darlington, Yue Ma, C. Ferrari, B. Andrieu, P Gyorgy, S Vetter, Z. Xu, M. Kobayashi, Y.-T. Lin, Y. Pan, S. Sharma
article en
7 citations

Abstract

Abstract This report describes the experimental strategy and technologies for XLZD, the next-generation xenon observatory sensitive to dark matter and neutrino physics. In the baseline design, the detector will have an active liquid xenon target of 60 tonnes, which could be increased to 80 tonnes if the market conditions for xenon are favorable. It is based on the mature liquid xenon time projection chamber technology used in current-generation experiments, LZ and XENONnT. The report discusses the baseline design and opportunities for further optimization of the individual detector components. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3 $$\sigma $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>σ</mml:mi> </mml:math> evidence potential for WIMP-nucleon cross sections as low as $$3\times 10^{-49}\mathrm \,cm^2$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mn>3</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>49</mml:mn> </mml:mrow> </mml:msup> <mml:mspace/> <mml:mi>c</mml:mi> <mml:msup> <mml:mi>m</mml:mi> <mml:mn>2</mml:mn> </mml:msup> </mml:mrow> </mml:math> (at 40 GeV/c $$^2$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mmultiscripts> <mml:mrow/> <mml:mrow/> <mml:mn>2</mml:mn> </mml:mmultiscripts> </mml:math> WIMP mass). The observatory will also have leading sensitivity to a wide range of alternative dark matter models. It is projected to have a 3 $$\sigma $$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>σ</mml:mi> </mml:math> observation potential of neutrinoless double beta decay of $$^{136}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mmultiscripts> <mml:mrow/> <mml:mrow/> <mml:mn>136</mml:mn> </mml:mmultiscripts> </mml:math> Xe at a half-life of up to $$5.7\times 10^{27}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mn>5.7</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>27</mml:mn> </mml:msup> </mml:mrow> </mml:math> years. Additionally, it is sensitive to astrophysical neutrinos from the sun and galactic supernovae.

The European Physical Journal CVol. 85(10)
Karlsruhe Institute of Technology (DE), University of Bern (CH), Roma Tre University (IT), Obayashi (Japan) (JP), Lawrence Livermore National Laboratory (US), Rutherford Appleton Laboratory (GB), The University of Sydney (AU), Pennsylvania State University (US), Bucknell University (US), St. George's University (GD), University of Wisconsin–Madison (US), Scuola Internazionale Superiore di Studi Avanzati (IT), University of Liverpool (GB), Lawrence Berkeley National Laboratory (US), University of Fribourg (CH), University of California, Santa Barbara (US), University of California, Los Angeles (US), Stockholm University (SE), The University of Melbourne (AU), Kavli Institute for the Physics and Mathematics of the Universe (JP), University of Groningen (NL), University of Alabama (US), Universidad de Granada (ES), University of Banja Luka (BA), John Brown University (US), King's College London (GB), Royal Holloway University of London (GB), South Dakota School of Mines and Technology (US), Johannes Gutenberg University Mainz (DE), Brookhaven National Laboratory (US), University of Ferrara (IT), University of Zurich (CH), Purdue University West Lafayette (US), Heidelberg University (DE), University of Münster (DE), University of Massachusetts Amherst (US), University of L'Aquila (IT), Brown University (US), University of Michigan (US), Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso (IT), Vatican Secret Archives (VA), SLAC National Accelerator Laboratory (US), Polytechnic Institute of Coimbra (PT), Westlake University (CN), Technische Universität Darmstadt (DE), University of Bristol (GB), University of California San Diego (US), Sorbonne Université (FR), University of Oxford (GB), University of Chicago (US), University of Belgrade (RS), ARC Centre of Excellence for Dark Matter Particle Physics (AU), National Institute for Subatomic Physics (NL), Kavli Institute for Particle Astrophysics and Cosmology (US), Sanford Research (US), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Basic Science (KR), Osservatorio Astrofisico di Torino (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Chinese University of Hong Kong, Shenzhen (CN), AlbaNova (SE), Institute of High Energy Physics (CN), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Gran Sasso Science Institute (IT), Max Planck Institute for Nuclear Physics (DE), Vitenparken (NO), Vatican Observatory (IT), Universidad de Londres (MX), South Dakota Science and Technology Authority (US), Laboratoire Médiations (FR), Institut des Sciences et technologies pour une Economie Circulaire des énergies bas carbone (FR), University College London (GB), Imperial College London (GB), University of Rochester (US), Weizmann Institute of Science (IL), Nagoya University (JP), Kobe University (JP), University of Maryland, College Park (US), Universitat de Barcelona (ES), Rice University (US), The University of Tokyo (JP), Black Hills State University (US), University of Coimbra (PT), Columbia University (US), Technische Universität Dresden (DE), University of California, Davis (US), The University of Texas at Austin (US), University of Sheffield (GB), University of Bologna (IT), University of California, Berkeley (US), Stanford University (US), Nantes Université (FR), University of Edinburgh (GB), Tsinghua University (CN)
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Dark Matter and Cosmic Phenomena
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