DarkSide search for dark matter

Alexander, T.; Alton, D.; Arisaka, K.; Back, H. O.; Beltrame, P.; Benziger, J.; Bonfini, G.; Brigatti, A.; Brodsky, J.; Bussino, S.; Cadonati, L.; Calaprice, F.; Candela, A.; Cao, Hua; Cavalcante, P.; Chepurnov, A.; Chidzik, S.; Cocco, A. G.; Condon, C.; D’Angelo, D.; Davini, S.; Vincenzi, M. De; Haas, E. de; Derbin, A.; Pietro, G. Di; Dratchnev, I.; Durben, Dan J.; Empl, A.; Etenko, A.; Fan, A.; Fiorillo, G.; Franco, D.; Fomenko, K.; Forster, G.; Gabriele, F.; Galbiati, C.; Gazzana, S.; Ghiano, C.; Goretti, A.; Grandi, L.; Gromov, M.; Guan, Mengyun; Guo, Cong; Guray, G.; Hungerford, E.; Ianni, A.; Ianni, An.; Joliet, C.; Kayunov, A.; Keeter, K. J.; Kendziora, C. L.; Kidner, S.; Klemmer, R.; Kobychev, V.; Koh, G.; Komor, M.; Korablëv, D.; Korga, G.; Li, P; Loer, B.; Lombardi, P.; Love, Christina; Ludhová, L.; Luitz, S.; Lukyanchenko, L.; Lund, Alan; Lung, K.; Ma, Y.; Machulin, I.; Mari, Stefano Maria; Maricic, J.; Martoff, C. J.; Meregaglia, A.; Meroni, E.; Meyers, P. D.; Mohayai, T.; Montanari, D.; Montuschi, M.; Monzani, M. E.; Mosteiro, P.; Mount, B. J.; Muratova, V.; Nelson, A.; Nemtzow, A.; Нурахов, Н. Н.; Orsini, M.; Ortica, F.; Pallavicini, M.; Pantic, E.; Parmeggiano, S.; Parsells, R.; Pelliccia, N.; Perasso, L.; Perasso, S.; Perfetto, F.; Pinsky, L.; Pocar, A.; Pordes, S.; Randle, K.; Ranucci, G.; Razeto, A.; Romani, A.; Rossi, B.; Rossi, N.; Rountree, S. D.; Saggese, Paolo; Saldanha, R.; Salvo, C.; Sands, W.; Seigar, Marc S.; Semenov, D.; Shields, E.; Skorokhvatov, M.; Smirnov, O.; Sotnikov, A.; Sukhotin, S.; Suvarov, Y; Tartaglia, R.; Tatarowicz, J.; Testera, G.; Thompson, J.; Tonazzo, A.; Unzhakov, E.; Vogelaar, R. B.; Wang, H; Westerdale, S.; Wójcik, Marcin; Wright, A.; Xu, J.; Yang, Changgen; Zavatarelli, S.; Zehfus, Michael; Zhong, Weili; Zuzel, G.

doi:10.1088/1748-0221/8/11/c11021

Cited by 39 publications

(27 citation statements)

References 8 publications

(9 reference statements)

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“…Signal processing of the acquired waveforms was achieved using a custom algorithm which was developed for background subtraction, timing, and pulse area determination. The algorithm is based upon that used in the DarkSide experiment [4] and its operation is illustrated in Figure 5. A moving average of the waveform data is taken as the baseline.…”

Section: Signal Processing Algorithmmentioning

confidence: 99%

Characterization and modeling of a Water-based Liquid Scintillator

et al. 2015

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We have characterised Water-based Liquid Scintillator (WbLS) using low energy protons, UV-VIS absorbance, and fluorescence spectroscopy. We have also developed and validated a simulation model that describes the behaviour of WbLS in our detector configurations for proton beam energies of 210 MeV, 475 MeV, and 2 GeV and for two WbLS compositions. Our results have enabled us to estimate the light yield and ionisation quenching of WbLS, as well as to understand the influence of the wavelength shifting of Cherenkov light on our measurements. These results are relevant to the suitability of WbLS materials for next generation intensity frontier experiments.

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Section: Signal Processing Algorithmmentioning

confidence: 99%

Characterization and modeling of a Water-based Liquid Scintillator

et al. 2015

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“…Ongoing dual-phase experiments include XENON100 [4,5], LUX [6,7] and PandaX-I [8,9] (all using LXe), as well as DarkSide-50 [10] (using LAr). While current dark matter detectors utilize up to a few hundred kg of LXe or LAr as their sensitive targets and probe the spinindependent WIMP-nucleon cross section down to 10 -45 -10 -46 cm 2 , ton-scale dual-phase experiments are already under construction or in different planning stages, e.g., XENON1T [11] (later to be upgraded to XENONnT), ArDM [12], LZ [13] and DarkSide G2 [10]; these are expected be sensitive to cross sections down to 10 -47 -10 -48 cm 2 . Multi-ton detectors, such as DARWIN [14], are foreseen to supersede these experiments in the next decade, reaching 10fold higher WIMP detection sensitivities, to the point where solar and atmospheric neutrinos will become the dominant background through coherent neutrino-nucleus scattering.…”

Section: Introductionmentioning

confidence: 99%

Liquid Hole Multipliers: bubble-assisted electroluminescence in liquid xenon

Arazi¹,

Erdal²,

Coimbra³

et al. 2015

J. Inst.

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In this work we discuss the mechanism behind the large electroluminescence signals observed at relatively low electric fields in the holes of a Thick Gas Electron Multiplier (THGEM) electrode immersed in liquid xenon. We present strong evidence that the scintillation light is generated in xenon bubbles trapped below the THGEM holes. The process is shown to be remarkably stable over months of operation, providing -under specific thermodynamic conditions -energy resolution similar to that of present dual-phase liquid xenon experiments. The observed mechanism may serve as the basis for the development of Liquid Hole Multipliers (LHMs), capable of producing local charge-induced electroluminescence signals in large-volume single-phase noble-liquid detectors for dark matter and neutrino physics experiments.

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“…1. Introduction 1,1,4,4-Tetraphenyl-1,3-Butadiene (TPB) is an organic compound commonly used as a wavelength shifter in a variety of particle experiments which employ noble liquids as the detector medium, including DEAP-3600 [1], MiniCLEAN [2], DarkSide [3], ArDM [4], WArP [5], nEDM at SNS [6], and MicroBooNE [7]. It converts the UV light emitted by the noble liquids to easier-to-detect visible light.…”

mentioning

confidence: 99%

Temperature dependence of alpha-induced scintillation in the 1,1,4,4-tetraphenyl-1,3-butadiene wavelength shifter

et al. 2016

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Liquid noble based particle detectors often use the organic wavelength shifter 1,1,4,4tetraphenyl-1,3-butadiene (TPB) which shifts UV scintillation light to the visible regime, facilitating its detection, but which also can scintillate on its own. Dark matter searches based on this type of detector commonly rely on pulse-shape discrimination (PSD) for background mitigation. Alphainduced scintillation therefore represents a possible background source in dark matter searches. The timing characteristics of this scintillation determine whether this background can be mitigated through PSD. We have therefore characterized the pulse shape and light yield of alpha induced TPB scintillation at temperatures ranging from 300 K down to 4 K, with special attention given to liquid noble gas temperatures. We find that the pulse shapes and light yield depend strongly on temperature. In addition, the significant contribution of long time constants above ∼50 K provides an avenue for discrimination between alpha decay events in TPB and nuclear-recoil events in noble liquid detectors.

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DarkSide search for dark matter

Cited by 39 publications

References 8 publications

Characterization and modeling of a Water-based Liquid Scintillator

Characterization and modeling of a Water-based Liquid Scintillator

Liquid Hole Multipliers: bubble-assisted electroluminescence in liquid xenon

Temperature dependence of alpha-induced scintillation in the 1,1,4,4-tetraphenyl-1,3-butadiene wavelength shifter

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