Preparation of neutron-activated xenon for liquid xenon detector calibration

Ni, Kan; Hasty, R.; Wongjirad, T.; Kastens, L.; Manzur, A.; McKinsey, D. N.

doi:10.1016/j.nima.2007.08.180

Cited by 17 publications

(18 citation statements)

References 15 publications

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“…Only isotopes with a very short half-life can be employed for regular calibrations, followed by science runs. Some of these sources are neutron-activated xenon, providing rather high-energy γ-lines at 164 keV ( 131m Xe, T 1/2 = 11.8 d) and 236 keV ( 129m Xe, T 1/2 = 8.9 d) [147]. However, the half-lives of the activated Xe isotopes are too long, and their energies too high, to be useful for ton-scale detectors.…”

Section: Calibrationmentioning

confidence: 99%

DARWIN: towards the ultimate dark matter detector

Aalbers

Agostini

Alfonsi

et al. 2016

J. Cosmol. Astropart. Phys.

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639

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DARk matter WImp search with liquid xenoN (DARWIN) will be an experiment for the direct detection of dark matter using a multi-ton liquid xenon time projection chamber at its core. Its primary goal will be to explore the experimentally accessible parameter space for Weakly Interacting Massive Particles (WIMPs) in a wide mass-range, until neutrino interactions with the target become an irreducible background. The prompt scintillation light and the charge signals induced by particle interactions in the xenon will be observed by VUV sensitive, ultra-low background photosensors. Besides its excellent sensitivity to WIMPs above a mass of 5 GeV/c(2), such a detector with its large mass, lowenergy threshold and ultra-low background level will also be sensitive to other rare interactions. It will search for solar axions, galactic axion-like particles and the neutrinoless double-beta decay of (136)Xe, as well as measure the low-energy solar neutrino flux with < 1% precision, observe coherent neutrinonucleus interactions, and detect galactic supernovae. We present the concept of the DARWIN detector and discuss its physics reach, the main sources of backgrounds and the ongoing detector design and RD; efforts.

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Section: Calibrationmentioning

confidence: 99%

DARWIN: towards the ultimate dark matter detector

Aalbers

Agostini

Alfonsi

et al. 2016

J. Cosmol. Astropart. Phys.

Self Cite

639

779

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“…The 9.4 and 32.1 keV de-excitations of 83m Kr [16] are not comprised solely of gamma rays, but are also included in the figure for completeness. Two points, at 164 and 236 keV (hollow blue crosses [34]), are from inelastic neutron scatters, resulting in gammas of these energies together with a nuclear recoil component, which may possibly serve to increase the yield. The right-hand y-axis uses the definition W ph = E dep /N ph , as described in the text.…”

Section: Zero-field Scintillation Yield Vs Energymentioning

confidence: 99%

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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“…In addition to the simulations, we also used neutron activated xenon isotopes, primarily 131m Xe (164 keV gammas) and 129m Xe (236 keV gammas) to calibrate the detector's S1 response throughout the entire active volume. The activated xenon isotopes were introduced into the XENON10 detector following several days of neutron activation of natural xenon [51]. Unlike external calibration sources, activated Xe isotopes provided unique energy and position calibration throughout the entire LXe sensitive volume.…”

Section: Position-dependence Of S1 and S2 Signalsmentioning

confidence: 99%

Design and performance of the XENON10 dark matter experiment

Aprile

Angle

Arneodo

et al. 2011

Astroparticle Physics

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120

184

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XENON10 is the first two-phase xenon time projection chamber (TPC) developed within the XENON dark matter search program. The TPC, with an active liquid xenon (LXe) mass of about 14 kg, was installed at the Gran Sasso Underground Laboratory (LNGS) in Italy, and operated for more than one year, with excellent stability and performance. Results from a dark matter search with XENON10 have been published elsewhere. In this paper, we summarize the design and performance of the detector and its subsystems, based on calibration data using sources of gamma-rays and neutrons as well as background and Monte Carlo simulation data. The results on the detector's energy threshold, position resolution, and overall efficiency show a performance that exceeds design specifications, in view of the very low energy threshold achieved (<10 keVr) and low background rate achieved.Design and Performance of the XENON10 Dark Matter Experiment XENON10 is the first two-phase xenon time projection chamber (TPC) developed within the XENON dark matter search program. The TPC, with an active liquid xenon (LXe) mass of about 14 kg, was installed at the Gran Sasso underground laboratory (LNGS) in Italy, and operated for more than one year, with excellent stability and performance. Results from a dark matter search with XENON10 have been published elsewhere. In this paper, we summarize the design and performance of the detector and its subsystems, based on calibration data using sources of gamma-rays and neutrons as well as background and Monte Carlo simulations data. The results on the detector's energy threshold, energy and position resolution, and overall efficiency show a performance that exceeds design specifications, in view of the very low energy threshold achieved (<10 keVr) and the excellent energy resolution achieved by combining the ionization and scintillation signals, detected simultaneously.PACS numbers: 95.35.+d, 29.40.Mc, 95.55.Vj

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Preparation of neutron-activated xenon for liquid xenon detector calibration

Cited by 17 publications

References 15 publications

DARWIN: towards the ultimate dark matter detector

DARWIN: towards the ultimate dark matter detector

NEST: a comprehensive model for scintillation yield in liquid xenon

Design and performance of the XENON10 dark matter experiment

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