Sensitivity and discovery potential of the proposed nEXO experiment to neutrinoless double-
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 decay

Albert, J.; Anton, G.; Arnquist, I. J.; Badhrees, I.; Barbeau, P. S.; Beck, D.; Belov, V.; Bourque, F.; Brodsky, J.; Brown, E.; Brunner, T.; Burenkov, A.; Cao, G. F.; Cao, Liqiang; Cen, W. R.; Chambers, Claire; Charlebois, Serge A.; Chiu, M.; Cleveland, B. T.; Coon, Minor J.; Craycraft, A.; Cree, W.; Cote, M.; Dalmasson, J.; Daniels, T.; Daugherty, S. J.; Daughhetee, J.; Delaquis, S.; Mesrobian-Kabakian, A. Der; DeVoe, R.; Didberidze, T.; Dilling, J.; Ding, Ying; Dolinski, M. J.; Dragone, A.; Fabris, L.; Fairbank, W. M.; Farine, J.; Feyzbakhsh, S.; Fontaine, R.; Fudenberg, D.; Giacomini, G.; Gornea, R.; Graham, K.; Gratta, G.; Hansen, E. V.; Harris, D. A.; Hasan, M. A.; Heffner, M.; Hoppe, E. W.; House, A.; Hufschmidt, P.; Hughes, M.; Hößl, J.; Ito, Yuta; Iverson, A.; Jamil, A.; Jewell, M. J.; Jiang, X. S.; Johnson, T. N.; Johnston, S.; Karelin, A.; Kaufman, L. J.; Killick, Ryan; Koffas, T.; Kravitz, S.; Krücken, R.; Kuchenkov, A.; Kumar, Krishna; Lan, Y.; Leonard, D. S.; Li, G.; Li, S.; Li, Z.; Licciardi, C.; Lin, Yi-Hsuan; MacLellan, R.; Michel, Thilo; Mong, B.; Moore, David C.; Murray, K.; Newby, J.; Ning, Z.; Njoya, O.; Nolet, F.; Odgers, K.; Odian, A.; Oriunno, M.; Orrell, J. L.; Ostrovskiy, I.; Overman, C.T.; Ortega, G. S.; Parent, Samuel; Piepke, A.; Pocar, A.; Pratte, J.‐F.; Qiu, Delong; Radeka, V.; Raguzin, Е.; Rao, T.; Rescia, S.; Retière, F.; Robinson, A.; Rossignol, T.; Rowson, P. C.; Roy, N.; Saldanha, R.; Sangiorgio, S.; Schmidt, Susann; Schneider, Judith; Schubert, A.; Sinclair, D.; Skarpaas, K.; Soma, A. K.; St-Hilaire, G.; Stekhanov, V.; Stiegler, T.; Sun, Xiangming; Tarka, M.; Todd, J.; Tolba, T.; Tsang, R.; Tsang, T.; Vachon, F.; Veeraraghavan, V.; Visser, G.; Vogel, P.; Vuilleumier, J. L.; Wagenpfeil, M.; Wang, Q.; Weber, M.; Wei, Wenlu; Wen, L.; Wichoski, U.; Wrede, Gerrit; Wu, Sen; Wu, W.; Yang, L.; Yen, Y.-R.; Zeldovich, O.; Zettlemoyer, J.; Zhang, X.; Zhao, Jianzhou; Zhou, Y.; Ziegler, T.

doi:10.1103/physrevc.97.065503

Cited by 198 publications

(206 citation statements)

References 61 publications

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“…This lifetime is sufficient to drift and collect charge in the current setup, which has a maximum drift time of 16.6 µs. In nEXO the expected electron lifetime is >10 ms but the ultimate drift length in nEXO is expected to be ∼625 µs [2] which is significantly larger than that achieved here. The approximate ratio of lifetime to drift length is still comparable making this representative of the expected purity effects in nEXO.…”

Section: Test Cellmentioning

confidence: 75%

“…The observation of this lepton-number-violating process would indicate that neutrinos are Majorana particles and could constrain the absolute neutrino mass scale [1]. The planned next-generation detector (nEXO) proposes to search for 0νββ decay of 136 Xe in a 5 tonne liquid xenon (LXe) time projection chamber (TPC) [2]. The nEXO experiment plans to build on the success of the currently operating EXO-200 experiment [3].…”

Section: Introductionmentioning

confidence: 99%

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Characterization of an Ionization Readout Tile for nEXO

et al. 2018

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A new design for the anode of a time projection chamber, consisting of a charge-detecting “tile", is investigated for use in large scale liquid xenon detectors. The tile is produced by depositing 60 orthogonal metal charge-collecting strips, 3 mm wide, on a 10 cm × 10 cm fused-silica wafer. These charge tiles may be employed by large detectors, such as the proposed tonne-scale nEXO experiment to search for neutrinoless double-beta decay. Modular by design, an array of tiles can cover a sizable area. The width of each strip is small compared to the size of the tile, so a Frisch grid is not required. A grid-less, tiled anode design is beneficial for an experiment such as nEXO, where a wire tensioning support structure and Frisch grid might contribute radioactive backgrounds and would have to be designed to accommodate cycling to cryogenic temperatures. The segmented anode also reduces some degeneracies in signal reconstruction that arise in large-area crossed-wire time projection chambers. A prototype tile was tested in a cell containing liquid xenon. Very good agreement is achieved between the measured ionization spectrum of a 207Bi source and simulations that include the microphysics of recombination in xenon and a detailed modeling of the electrostatic field of the detector. An energy resolution σ/E=5.5% is observed at 570 keV, comparable to the best intrinsic ionization-only resolution reported in literature for liquid xenon at 936 V/cm.

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Section: Test Cellmentioning

confidence: 75%

Section: Introductionmentioning

confidence: 99%

Characterization of an Ionization Readout Tile for nEXO

et al. 2018

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“…One sees that m ββ is determined within rather small errors, and presents a challenge for the next generation of 0νββ searches. For comparison, the top green horizontal band in Figure 2 represents the current experimental limits from Kamland-Zen (61 − 165 meV) [33], while the dashed horizontal lines correspond to the projected most optimistic sensitivities from LEGEND (10.7 − 22.8 meV) [34], SNO + Phase II (19 − 46 meV) [35], and nEXO (5.7 − 17.7 meV) [36].…”

Section: E Neutrinoless Double Beta Decaymentioning

confidence: 99%

Flavour and CP predictions from orbifold compactification

2020

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We propose a theory for fermion masses and mixings in which an A4 family symmetry arises naturally from a six-dimensional spacetime after orbifold compactification. The flavour symmetry leads to the successful "golden" quark-lepton unification formula and the possibility of "geometrical" CP violation. The model reproduces oscillation parameters with good precision, giving sharp predictions for the CP violating phases of quarks and leptons, in particular δ +268 • . The effective neutrinoless double-beta decay mass parameter is also sharply predicted as m ββ 2.65

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“…The widths of these bands reflect uncertainties in nuclear matrix elements. The lower bands show the future sensitives from LEGEND (10.7 − 22.8 meV) [39], SNO + Phase II (19 − 46 meV) [40] and nEXO (5.7 − 17.7 meV) [41].…”

Section: Whether Neutrinos Are Majorana or Dirac Fermions Is Still Anmentioning

confidence: 99%

A theory for scotogenic dark matter stabilised by residual gauge symmetry

et al. 2020

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Dark matter stability can result from a residual matter-parity symmetry, following naturally from the spontaneous breaking of the gauge symmetry. Here we explore this idea in the context of the SU(3)c ⊗ SU(3)L ⊗ U(1)X ⊗ U(1)N electroweak extension of the standard model. The key feature of our new scotogenic dark matter theory is the use of a triplet scalar boson with anti-symmetric Yukawa couplings. This naturally implies that one of the light neutrinos is massless and, as a result, there is a lower bound for the 0νββ decay rate. I. INTRODUCTIONIn order to account for the existence of cosmological dark matter, we need new particles not present in the Standard Model (SM) of particle physics. Moreover, new symmetries capable of stabilising the corresponding candidate particle on cosmological scales are also required. Here we focus on the so-called Weakly Interacting Massive Particles, or WIMPs, as dark matter candidates. Within supersymmetric schemes, WIMP stability follows from having a conserved R-parity symmetry [1]. Our present construction does not rely on supersymmetry nor on the imposition of any ad hoc symmetry to stabilise dark matter. It is also a more complete theory setup, in the sense that it naturally generates neutrino masses as well. These arise radiatively, thanks to the exchange of new particles in the "dark" sector. The procedure is very well-motivated since neutrino masses are anyways necessary to account for neutrino oscillation data [2].Here we follow an alternative approach that naturally incorporates neutrino mass right from the beginning. This is provided by scotogenic dark matter schemes. These are "low-scale" models of neutrino mass [3] where dark matter emerges as a radiative mediator of neutrino mass generation. In this case, the symmetry stabilising dark matter is also responsible for the radiative origin of neutrino masses in a very elegant way [4]. Yet, in this case too, a dark matter stabilisation symmetry is introduced in an ad hoc manner. The need for such "dark" symmetry is a generic feature also of other scotogenic schemes, such as the generalization proposed in [5,6].Extending the SU(3) c ⊗ SU(2) L ⊗ U(1) Y gauge symmetry can provide a natural setting for a theory of dark matter where stabilisation can be automatic [7][8][9]. Such electroweak extensions involve the SU(3) L gauge symmetry, which also provides an "explanation" of the number of quark and lepton families from the anomaly cancellation requirement [10][11][12]. For recent papers using the SU(3) L gauge symmetry see . These theories can also, in

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Sensitivity and discovery potential of the proposed nEXO experiment to neutrinoless double- β decay

Cited by 198 publications

References 61 publications

Characterization of an Ionization Readout Tile for nEXO

Characterization of an Ionization Readout Tile for nEXO

Flavour and CP predictions from orbifold compactification

A theory for scotogenic dark matter stabilised by residual gauge symmetry

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