English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Zendy Open

Presents the pdf analysis as premium feature

PDF Analysis

Insights

Presents the summarisation as premium feature

Summarisation

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the zaia usage as premium feature

ZAIA

Zendy Tools

Zendy Plus

Presents the access of premium content as premium feature

Premium Content

We study a three stage dark matter and neutrino observatory based onmulti-ton two-phase liquid Xe and Ar detectors with sufficiently lowbackgrounds to be sensitive to WIMP dark matter interaction cross sections downto 10E-47 cm^2, and to provide both identification and two independentmeasurements of the WIMP mass through the use of the two target elements in a5:1 mass ratio, giving an expected similarity of event numbers. The samedetection systems will also allow measurement of the pp solar neutrinospectrum, the neutrino flux and temperature from a Galactic supernova, andneutrinoless double beta decay of 136Xe to the lifetime level of 10E27 - 10E28y corresponding to the Majorana mass predicted from current neutrinooscillation data. The proposed scheme would be operated in three stages G2, G3,G4, beginning with fiducial masses 1-ton Xe + 5-ton Ar (G2), progressing to10-ton Xe + 50-ton Ar (G3) then, dependent on results and performance of thelatter, expandable to 100-ton Xe + 500-ton Ar (G4). This method of scale-upoffers the advantage of utilizing the Ar vessel and ancillary systems of onestage for the Xe detector of the succeeding stage, requiring only one newdetector vessel at each stage. Simulations show the feasibility of reducing orrejecting all external and internal background levels to a level <1 events peryear for each succeeding mass level, by utilizing an increasing outer thicknessof target material as self-shielding. The system would, with increasing massscale, become increasingly sensitive to annual signal modulation, the agreementof Xe and Ar results confirming the Galactic origin of the signal. Dark mattersensitivities for spin-dependent and inelastic interactions are also included,and we conclude with a discussion of possible further gains from the use ofXe/Ar mixtures.

Studies of a three-stage dark matter and neutrino observatory based on multi-ton combinations of liquid xenon and liquid argon detectors