Liquid xenon detector for dark matter search at Gran Sasso

Belli, P.; Bernabei, R.; Dai, C. J.; Incicchitti, A.; Prosperi, D.; Bacci, C.

doi:10.1016/0168-9002(93)91118-7

Cited by 30 publications

(6 citation statements)

References 19 publications

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“…They may be explained by nonuniform light collection in the detector, as claimed by [36]. Also discarded, for the purpose of our plot and the optimization, was one result considerably distant from all others, quoting less than 34 photons/keV at 22 and 88 keV [39]. Below 15 keV, the Thomas-Imel box model dominates, and it is in this regime where we find the optimal value for ξ /N i .…”

Section: Zero-field Scintillation Yield Vs Energymentioning

confidence: 80%

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NEST: a comprehensive model for scintillation yield in liquid xenon

et al. 2011

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A comprehensive model for explaining scintillation yield in liquid xenon is introduced. We unify various definitions of work function which abound in the literature and incorporate all available data on electron recoil scintillation yield. This results in a better understanding of electron recoil, and facilitates an improved description of nuclear recoil. An incident gamma energy range of O(1 keV) to O(1 MeV) and electric fields between 0 and O(10 kV/cm) are incorporated into this heuristic model. We show results from a Geant4 implementation, but because the model has a few free parameters, implementation in any simulation package should be simple. We use a quasi-empirical approach, with an objective of improving detector calibrations and performance verification. The model will aid in the design and optimization of future detectors. This model is also easy to extend to other noble elements. In this paper we lay the foundation for an exhaustive simulation code which we call NEST (Noble Element Simulation Technique).

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Section: Zero-field Scintillation Yield Vs Energymentioning

confidence: 80%

“…This work function is also known as W ph[9] or W s[39], conflicting with others' use of the same nomenclature[26].…”

mentioning

confidence: 94%

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NEST: a comprehensive model for scintillation yield in liquid xenon

et al. 2011

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“…This trend can be observed both in LXe and LAr. According [108]; e) [75]; f ) [104]; g) [109]; h) [110]; i) [111]; j) [112]; k) [113]; l) [114]; m) [115]; n) [116]. p) Using measured scintillation efficiency referred to 122 keV γ-rays [117] and W min s from [73].…”

Section: Emission Mechanism and Yieldsmentioning

confidence: 99%

Liquid noble gas detectors for low energy particle physics

2013

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We review the current status of liquid noble gas radiation detectors with energy threshold in the keV range, which are of interest for direct dark matter searches, measurement of coherent neutrino scattering and other low energy particle physics experiments. Emphasis is given to the operation principles and the most important instrumentation aspects of these detectors, principally of those operated in the double-phase mode. Recent technological advances and relevant developments in photon detection and charge readout are discussed in the context of their applicability to those experiments.

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“…Electrons can be produced by natural radioactivities and cosmic rays but estimations show that such processes will be negligible if the detector will be placed in a proper underground environment and the purity of xenon will be kept on a sufficient level. Xenon is an inert gas which can be purified to the level of better than 1 ppb (residual oxygen less than 0.1 ppb) [29], [30].…”

Section: Cross Sections and Capture Ratesmentioning

confidence: 99%

A xenon solar neutrino detector

Georgadze¹,

Klapdor‐Kleingrothaus²,

Päs³

et al. 1999

Nuclear Physics B - Proceedings Supplements

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The neutrino capture by 131 Xe with a threshold at 352 keV as reaction to detect solar neutrinos is examined. The most important feature of this process is its high sensitivity to beryllium neutrinos, which contribute approximately 40% to the total capture rate (45 SNU) assuming the fluxes predicted by the Standard Solar Model of [3]. The procedure of extraction of the daughter cesium atoms from liquid xenon as well as other technical problems concerning preparation of the cesium sample, low background measurements and side reactions for a possible realisation as a solar neutrino detector are discussed. The expected counting rate according to the SSM of [3] for a 131 Xe detector is ≈ 1500 events/y·kton. The results of such a detector will be important for solving the puzzle of the possible existence of vacuum oscillations or the MSW effect and/or input parameters of the Standard Solar Models.

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Liquid xenon detector for dark matter search at Gran Sasso

Cited by 30 publications

References 19 publications

NEST: a comprehensive model for scintillation yield in liquid xenon

NEST: a comprehensive model for scintillation yield in liquid xenon

Liquid noble gas detectors for low energy particle physics

A xenon solar neutrino detector

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