New technique for the measurement of the scintillation efficiency of nuclear recoils

Ninković, J.; Christ, P.; Angloher, G.; Hauff, D.; Huff, P.; Pantic, E.; Petricca, F.; Pröbst, F.; Seidel, W.

doi:10.1016/j.nima.2006.04.039

Cited by 22 publications

(18 citation statements)

References 14 publications

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“…Remembering that the kB values could be different under different experimental conditions and data treatment, we will use R ′ i for H to determine kB in this particular measurements and will use this kB value to calculate R ′ i for all other ions. Value of kB = 17 × 10 −3 g MeV −1 cm −2 gives R ′ H = 2.17 that well reproduces values for H given in Table 4 of [43] (2.15 ± 0.02 for collection of the scintillation signal during ∆t = 40 µs, and 2.18 ± 0.02 for ∆t = 50 µs). R ′ i values for other ions calculated with this kB value are shown in Fig.…”

Section: Cawosupporting

confidence: 82%

“…10a together with experimental results 12 of Ref. [43] in dependence on ion's Z number. Theoretical points lay on smooth curve well fitted by polynomial R ′ i (Z) = a + bZ + cZ 2 with a = 0.87098, b = 0.98708 and c = −5.9896 × 10 −3 (also shown in Fig.…”

Section: Cawomentioning

confidence: 57%

“…(4) Dependence of the light output and quenching factors in CaWO 4 on atomic mass of ion was measured in Ref. [43] by impinging various ions -from H to Au -onto the scintillating crystal. All ions had energy of 18 keV.…”

Section: Cawomentioning

confidence: 99%

“…(6), normalized to that of electrons at 6 keV, were calculated and presented in Table 4 of Ref. [43]:…”

Section: Cawomentioning

confidence: 99%

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Semi-empirical calculation of quenching factors for ions in scintillators

Tretyak

2010

Astroparticle Physics

215

249

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Semi-empirical method of calculation of quenching factors for scintillators is described. It is based on classical Birks formula with the total stopping powers for electrons and ions which are calculated with the ESTAR and SRIM codes, respectively. Method has only one fitting parameter (the Birks factor kB) which can have different values for the same material in different conditions of measurements and data treatment. A hypothesis is used that, once the kB value is obtained by fitting data for particles of one kind and in some energy region (e.g. for a few MeV α particles from internal contamination of a detector), it can be applied to calculate quenching factors for particles of another kind and for another energies (e.g. for low energy nuclear recoils) if all data are measured in the same experimental conditions and are treated in the same way. Applicability of the method is demonstrated on many examples including materials with different mechanisms of scintillation: organic scintillators (solid C 8 H 8 , and liquid C 16 H 18 , C 9 H 12 ); crystal scintillators (pure CdWO 4 , PbWO 4 , ZnWO 4 , CaWO 4 , CeF 3 , and doped CaF 2 (Eu), CsI(Tl), CsI(Na), NaI(Tl)); liquid noble gases (LXe). Estimations of quenching factors for nuclear recoils are also given for some scintillators where experimental data are absent (CdWO 4 , PbWO 4 , CeF 3 , Bi 4 Ge 3 O 12 , LiF, ZnSe).

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Section: Cawosupporting

confidence: 82%

Section: Cawomentioning

confidence: 57%

Section: Cawomentioning

confidence: 99%

“…(6), normalized to that of electrons at 6 keV, were calculated and presented in Table 4 of Ref. [43]:…”

Section: Cawomentioning

confidence: 99%

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Semi-empirical calculation of quenching factors for ions in scintillators

Tretyak

2010

Astroparticle Physics

215

249

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“…Since the resolution of light-detectors operated in the CRESST setup at present is not sufficient to disentangle O, Ca and W recoils unambiguously, dedicated experiments to measure the QFs of CaWO 4 are necessary. Earlier attempts yield inconclusive results, in particular for the value of QF W [27,28,29]. [31].…”

Section: Quenching Factors (Qfs)mentioning

confidence: 99%

Energy-dependent light quenching in CaWO $$_4$$ 4 crystals at mK temperatures

et al. 2014

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Scintillating CaWO 4 single crystals are a promising multi-element target for rare-event searches and are currently used in the direct dark matter experiment CRESST (Cryogenic Rare Event Search with Superconducting Thermometers). The relative light output of different particle interactions in CaWO 4 is quantified by quenching factors (QFs). These are essential for an active background discrimination and the identification of a possible signal induced by weakly interacting massive particles (WIMPs). We present the first precise measurements of the QFs of O, Ca and W at mK temperatures by irradiating a cryogenic detector with a fast neutron beam. A clear energy dependence of the QF of O and, less pronounced, of Ca was observed for the first time. Furthermore, in CRESST neutron-calibration data a variation of the QFs among different CaWO 4 single crystals was found. For typical CRESST detectors the QFs in the region-of-interest (10-40 keV) are QF ROI O = (11.2 ± 0.5) %, QF ROI Ca = (5.94±0.49) % and QF ROI W = (1.72±0.21) %. The latest CRESST data (run32) is reanalyzed using these fundamentally new results on light quenching in CaWO 4 having moderate influence on the WIMP analysis. Their relevance for future CRESST runs and for the clarification of previa

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Cryogenic Detectors

Pretzl¹

2020

Particle Physics Reference Library

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Most calorimeters used in high energy physics measure the energy loss of a particle in form of ionization (free charges) or scintillation light. However, a large fraction of the deposited energy in form of heat remains undetected. The energy resolution of these devices is therefore mainly driven by the statistical fluctuations of the number of charge carriers or photoelectrons involved in an event. In contrast, cryogenic calorimeters are able to measure the total deposited energy including the heat in form of phonons or quasi-particles in a superconductor. With the appropriate phonon or quasi-particle detection system much higher energy resolutions can be obtained due to the very large number of low energy quanta (meV) involved in the process. This feature makes cryogenic calorimeters very effective in the detection of very small energy deposits (eV) with resolutions more than an order of magnitude better than for example semiconductor devices. During the last two decades cryogenic detectors have been developed to explore new frontiers in physics and astrophysics. Among these are the quest for the dark matter in the universe, the neutrinoless double beta decay and the mass of the neutrino. But other fields of research have also benefited from these developments, such as astrophysics, material and life sciences. The calorimetric measurement of deposited energy in an absorber dates back to 1878, when the American astronomer S.P. Langley invented the bolometer [1]. With this device he was able to measure the energy flow of the sun in the far infrared region of the spectrum and to determine the solar constant. Since then the bolometer has played an important role to measure the energy of electromagnetic radiation

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New technique for the measurement of the scintillation efficiency of nuclear recoils

Cited by 22 publications

References 14 publications

Semi-empirical calculation of quenching factors for ions in scintillators

Semi-empirical calculation of quenching factors for ions in scintillators

Energy-dependent light quenching in CaWO $$_4$$ 4 crystals at mK temperatures

Cryogenic Detectors

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