Study of the internal background of CsI(Tℓ) crystal detectors for dark matter search

Kim, T.Y; Cho, I.S; Choi, Do Lim; Choi, Jong-San; Hahn, I. S.; Hwang, Mun Kyung; Jang, H. K.; Jain, R. K.; Kang, Ung Gu; Kim, H.J; Kim, J.H; Kim, S.C; Kim, Y.D; Kwon, Y.; Lee, H.S; Lee, J.H; Lee, M.H; Lee, S.E; Noh, S. H.; Park, Hyojin; Park, I.H; Seo, E. S.; Won, E.; Won, Hayoun; Yang, H.Y.; Yang, M. S.; Yu, I.

doi:10.1016/s0168-9002(03)00346-2

Cited by 36 publications

(11 citation statements)

References 11 publications

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“…Major internal backgrounds for β-decays in our CsI(Tl) crystals are 137 Cs (Q=1175.6 keV), 134 Cs (Q=2058.7 keV) and 87 Rb (Q=282 keV). The energy spectra from those radioisotopes are flat in our search region, 2 keV to 12 keV, as from Compton-scattered γ rays in the MD events [31,32]. Therefore we expect that the MD energy spectrum is similar to the R e − spectrum in the SD sample.…”

Section: Discussionmentioning

confidence: 71%

“…Since an axion would give rise to an electron-like signal with a hit in only a single detectormodule, only SD events were selected as axion candidate events. The SD events include surface α events (S α ) and electron recoil events (R e − ) from Compton scattered γ rays and β decays in the crystal bulk [31,32]. The S α events come from decays of radioactive isotopes which contaminate the surfaces of the crystals or the surrounding materials.…”

Section: Discussionmentioning

confidence: 99%

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Search for solar axions with CsI(Tl) crystal detectors

Yoon

Park

Bhang

et al. 2016

J. High Energ. Phys.

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Abstract:The results of a search for solar axions from the Korea Invisible Mass Search (KIMS) experiment at the Yangyang Underground Laboratory are presented. Low-energy electron-recoil events would be produced by conversion of solar axions into electrons via the axio-electric effect in CsI(Tl) crystals. Using data from an exposure of 34,596 kg · days, we set a 90 % confidence level upper limit on the axion-electron coupling, g ae , of 1.39 × 10 −11 for an axion mass less than 1 keV/c 2 . This limit is lower than the indirect solar neutrino bound, and fully excludes QCD axions heavier than 0.48 eV/c 2 and 140.9 eV/c 2 for the DFSZ and KSVZ models respectively.

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Section: Discussionmentioning

confidence: 71%

Section: Discussionmentioning

confidence: 99%

Search for solar axions with CsI(Tl) crystal detectors

Yoon

Park

Bhang

et al. 2016

J. High Energ. Phys.

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“…[22], this degree of improvement is achievable through the application of additional shielding and well-understood techniques to reduce the dominant internal radiocontaminations of CsI [33] (see also Refs. [34][35][36]). We also include in our analysis an overall systematic uncertainty of ±28% on the overall signal rate, corresponding to uncertainties associated with the cross section, detector efficiency, and overall neutrino flux.…”

Section: Projected Sensitivity To Sterile Neutrinosmentioning

confidence: 99%

Constraining sterile neutrino interpretations of the LSND and MiniBooNE anomalies with coherent neutrino scattering experiments

Blanco

Machado

2020

Phys. Rev. D

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Results from the LSND and MiniBooNE experiments have been interpreted as evidence for a sterile neutrino with a mass near the electronvolt scale. Here we propose to test such a scenario by measuring the coherent elastic scattering rate of neutrinos from a pulsed spallation source. Coherent scattering is universal across all active neutrino flavors, and thus can provide a measurement of the total Standard Model neutrino flux. By performing measurements over different baselines and making use of timing information, it is possible to significantly reduce the systematic uncertainties and to independently measure the fluxes of neutrinos that originate as νµ or as either νe orνµ. We find that a 100 kg CsI detector would be sensitive to the large fraction of the sterile neutrino parameter space that could potentially account for the LSND and MiniBooNE anomalies.

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“…The dashed black line represents the gain to which all PMTs were matched. The high voltage chosen for each PMT is given inTable 5.1.Before assembly the gain curve of each ET 9102SB was mapped by attaching each PMT to the same crystal and irradiating the setup with a57 Co source, which provides γs with an energy of 122 keV. An Amptek MCA 8000A (Pocket MCA) was used to record the energy spectrum for each PMT operated at several different high voltages.…”

mentioning

confidence: 99%

“…K, 126 I and134, 137 Cs, when grown from appropriate salts[57]. In her PhD thesis[42], Nicole Fields screened a boule slice of CsI[Na] from AMCRYS-H using low-background γ…”

mentioning

confidence: 99%