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

Aalbers J; Abe K; Adrover M; Maouloud SA; Akerib DS; Al Musalhi AK; Alder F; Althueser L; Amaral DWP; Amarasinghe CS; Ames A; Andrieu B; Angelides N; Angelino E; Antunovic B; Aprile E; Araujo HM; Armstrong JE; Arthurs M; Babicz M; Baker A; Balzer M; Bang J; Barberio E; Bargemann JW; Barillier E; Basharina-Freshville A; Baudis L; Bauer D; Bazyk M; Beattie K; Beaupere N; Bell NF; Bellagamba L; Benson T; Bhatti A; Biesiadzinski TP; Biondi R; Biondi Y; Birch HJ; Bishop E; Bismark A; Boehm C; Boese K; Bolotnikov A; Bras P; Braun R; Breskin A; Brew CAJ; Brommer S; Brown A; Bruni G; Budnik R; Burdin S; Cai C; Capelli C; Carini G; Carmona-Benitez MC; Chauvin A; Carter M; Chawla A; Chen H; Cherwinka JJ; Chin YT; Chott NI; Chavez APC; Clark K; Colijn AP; Colling DJ; Conrad J; Converse MV; Cooper LJ; Coronel R; Costanzo D; Cottle A; Cox G; Cuenca-Garcia JJ; Curran D; Cussans D; D'Andrea V; Garcia LCD; Darlington I; Dave S; David A; Davies GJ; Decowski MP; Deisting A; Delgaudio J; Dey S; Di Donato C; Di Felice L; Di Gangi P; Diglio S; Ding C; Dobson JEY; Doerenkamp M; Drexlin G; Druszkiewicz E; Dunbar CL; Eitel K; Elykov A; Engel R; Eriksen SR; Fayer S; Fearon NM; Ferella AD; Ferrari C; Fieldhouse N; Fischer H; Flaecher H; Flehmke T; Flierman M; Fraser ED; Fruth TMA; Fujikawa K; Fulgione W; Fuselli C; Gaemers P; Gaior R; Gaitskell RJ; Gallice N; Galloway M; Gao F; Garroum N; Geffre A; Genovesi J; Ghag C; Ghosh S; Giacomobono R; Gibbons R; Girard F; Glade-Beucke R; Glueck F; Gokhale S; Grandi L; Green J; Grigat J; Grinten MGD; Grossle R; Guan H; Guida M; Gyorgy P; Haiston JJ; Hall CR; Hall T; Hammann R; Hannen V; Hansmann-Menzemer S; Hargittai N; Hartigan-O'Connor E; Haselschwardt SJ; Hernandez M; Hertel SA; Higuera A; Hils C; Hiraoka K; Hoetzsch L; Hoferichter M; Homenides GJ; Hood NF; Horn M; Huang DQ; Hughes S; Hunt D; Iacovacci M; Itow Y; Jacquet E; Jakob J; James RS; Joerg F; Jones S; Kaboth AC; Kahlert F; Kamaha AC; Kaminaga Y; Kara M; Kavrigin P; Kazama S; Keller M; Kemp-Russell P; Khaitan D; Kharbanda P; Kilminster B; Kim J; Kirk R; Kleifges M; Klute M; Kobayashi M; Kodroff D; Koke D; Kopec A; Korolkova E; Kraus H; Kravitz S; Kreczko L; Krosigk B; Kudryavtsev VA; Kuger F; Kurita N; Landsman H; Lang RF; Lawes C; Lee J; Lehnert B; Leonard DS; Lesko KT; Levinson L; Li A; Li I; Li S; Liang S; Liang Z; Lin J; Lin Y-; Lindemann S; Linden S; Lindner M; Lindote A; Lippincott WH; Liu K; Loizeau J; Lombardi F; Lopes JAM; Lopes MI; Lorenzon W; Loutit M; Lu C; Lucchetti GM; Luce T; Luitz S; Ma Y; Macolino C; Mahlstedt J; Maier B; Majewski PA; Manalaysay A; Mancuso A; Manenti L; Mannino RL; Marignetti F; Marley T; Undagoitia TM; Martens K; Masbou J; Masson E; Mastroianni S; Maupin C; Mazza V; McCabe C; McCarthy ME; McKinsey DN; McLaughlin JB; Melchiorre A; Menendez J; Messina M; Miller EH; Milosovic B; Milutinovic S; Miuchi K; Miyata R; Mizrachi E; Molinario A; Monteiro CMB; Monzani ME; Mora K; Moriyama S; Morrison E; Morteau E; Mosbacher Y; Mount BJ; Mueller J; Murdy M; Murphy ASJ; Murra M; Naylor A; Nelson HN; Neves F; Newstead JL; Nguyen A; Ni K; O'Dell J; O'Hare C; Oberlack U; Obradovic M; Olcina I; Oliver-Mallory KC; Orebi Gann GD; Orpwood J; Ouahada S; Oyulmaz K; Paetsch B; Palladino KJ; Palmer J; Pan Y; Pandurovic M; Pannifer NJ; Paramesvaran S; Patton J; Pellegrini Q; Penning B; Pereira G; Peres R; Perry E; Pershing T; Piastra F; Pienaar J; Piepke A; Pierre M; Plante G; Pollmann TR; Pompa F; Principe L; Qi J; Qiao K; Qie Y; Qin J; Radeka S; Radeka V; Rajado M; Garcia DR; Ravindran A; Razeto A; Reichenbacher J; Rhyne CA; Richards A; Rischbieter GRC; Riyat HS; Rosero R; Roy A; Rushton T; Rynders D; Saakyan R; Sanchez L; Sanchez-Lucas P; Santone D; Santos JMF; Sartorelli G; Sazzad ABMR; Scaffidi A; Schnee RW; Schreiner J; Schulte P; Eissing HS; Schumann M; Schwenck A; Schwenk A; Lavina LS; Selvi M; Semeria F; Shagin P; Sharma S; Shaw S; Shen W; Sherman L; Shi S; Shi SY; Shimada T; Shutt T;

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 evidence potential for WIMP-nucleon cross sections as low as (at 40 GeV/c 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 observation potential of neutrinoless double beta decay of Xe at a half-life of up to  years. Additionally, it is sensitive to astrophysical neutrinos from the sun and galactic supernovae.