Quenching factor measurement for NaI(Tl) scintillation crystal

Joo, H. W.; Park, H.S.; Kim, J.H.; Lee, J.Y.; Kim, S.K.; Kim, Y.D.; Lee, H.S.; Kim, S.H.

doi:10.1016/j.astropartphys.2019.01.001

Cited by 60 publications

(64 citation statements)

References 22 publications

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“…This calibration setup was utilized in [6] to observe a monotonically decreasing QF with decreasing Na recoil energy in NaI[Tl], a trend at the time in tension with previous measurements. This behavior was later confirmed in four independent experiments [10][11][12][13].…”

Section: New Measurement Of the Quenching Factor For Csi[na]mentioning

confidence: 57%

Response of CsI[Na] to nuclear recoils: Impact on coherent elastic neutrino-nucleus scattering

2019

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A new measurement of the quenching factor for low-energy nuclear recoils in CsI[Na] is presented. Past measurements are revisited, identifying and correcting several systematic effects. The resulting global data are well-described by a physics-based model for the generation of scintillation by ions in this material, in agreement with phenomenological considerations. The uncertainty in the new model is reduced by a factor of four with respect to an energy-independent quenching factor initially adopted as a compromise by the COHERENT collaboration. A significantly improved agreement with Standard Model predictions for the first measurement of CEνNS is generated. We emphasize the critical impact of the quenching factor on the search for new physics via CEνNS experiments.

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Section: New Measurement Of the Quenching Factor For Csi[na]mentioning

confidence: 57%

Response of CsI[Na] to nuclear recoils: Impact on coherent elastic neutrino-nucleus scattering

2019

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“…It is worth noting that recently Ref. [45] gave quenching factors for a small COSINE-100 like detector; in particular: Na quenching factor ranging from 0.1 to 0.23 with a significant energy dependence, and I quenching factor ranging from 0.04 to 0.06 were reported; a very high precision is quoted. However, these values cannot be consistently considered for other detectors because of the above mentioned arguments; in particular, those crystals have been grown by different technique and protocols than those of DAMA/LIBRA.…”

Section: The Case Of Dm Particles Inducing Nuclear Recoilsmentioning

confidence: 86%

Improved model-dependent corollary analyses after the first six annual cycles of DAMA/LIBRA-phase2

Bernabei¹,

Belli²,

Cappella³

et al. 2019

Nucl. Phys. At. Energy

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Several of the many proposed Dark Matter candidate particles, already investigated with lower exposure and a higher software energy threshold, are further analyzed including the first DAMA/LIBRA-phase2 data release, with an exposure of 1.13 ton × yr and a lower software energy threshold (1 keV). The cumulative exposure above 2 keV considering also DAMA/NaI and DAMA/LIBRA-phase1 results is now 2.46 ton × yr. The analysis permits to constraint the parameters' space of the considered candidates restricting their values -with respect to previous analyses -thanks to the increase of the exposure and to the lower energy threshold.1 Throughout this paper keV means keV electron equivalent, where not otherwise specified.

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“…They are related by E ee = QE r , where Q is the quenching factor. DAMA/LIBRA have historically used the values Q = 0.3 and 0.09 for Na and I respectively [176], but we use the lower value Q = 0.1 for Na to reflect more recent measurements [177]. To account for the finite PMT resolution, we convolve Figure. The left-hand column shows the calculation ignoring gravitational focusing whereas the middle column shows the non-sinusoidal modifications that it gives rise to when it is included.…”

Section: A Modulation Signalsmentioning

confidence: 99%

Velocity substructure from Gaia and direct searches for dark matter

et al. 2020

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Data from the Gaia satellite show that the solar neighbourhood of the Milky Way's stellar halo is imprinted with substructure from several accretion events. Evidence of these events is found in "the Shards", stars clustering with high significance in both action space and metallicity. Stars in the Shards share a common origin, likely as ancient satellite galaxies of the Milky Way, so will be embedded in dark matter (DM) counterparts. These "Dark Shards" contain two substantial streams (S1 and S2), as well as several retrograde, prograde and lower energy objects. The retrograde stream S1 has a very high Earth-frame speed of ∼ 550 km s −1 while S2 moves on a prograde, but highly polar orbit and enhances peak of the speed distribution at around 300 km s −1 . The presence of the Dark Shards locally leads to modifications of many to the fundamental properties of experimental DM signals. The S2 stream in particular gives rise to an array of effects in searches for axions and in the time dependence of nuclear recoils: shifting the peak day, inducing non-sinusoidal distortions, and increasing the importance of the gravitational focusing of DM by the Sun. Dark Shards additionally bring new features for directional signals, while also enhancing the DM flux towards Cygnus.

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Quenching factor measurement for NaI(Tl) scintillation crystal

Cited by 60 publications

References 22 publications

Response of CsI[Na] to nuclear recoils: Impact on coherent elastic neutrino-nucleus scattering

Response of CsI[Na] to nuclear recoils: Impact on coherent elastic neutrino-nucleus scattering

Improved model-dependent corollary analyses after the first six annual cycles of DAMA/LIBRA-phase2

Velocity substructure from Gaia and direct searches for dark matter

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