EMI, the counting efficiency for electron capture, electron capture-gamma and isomeric transitions

Carles, A. Grau; Malonda, A. Grau; Carles, Pilar Grau

doi:10.1016/0010-4655(94)90234-8

Cited by 41 publications

(8 citation statements)

References 21 publications

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“…The results agree in relative intensity at 1% level. More recent measurements of the 210 Bi spectrum have been performed using Cherenkov and scintillator light detectors [82], [81]. The discrepancy between the β spectrum obtained from the scintillator measurement, also shown in Fig.…”

Section: The Pep and Cno Neutrino Interaction Ratesmentioning

confidence: 99%

Final results of Borexino Phase-I on low-energy solar neutrino spectroscopy

Bellini¹,

Benziger²,

Bick³

et al. 2014

Phys. Rev. D

289

345

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Borexino has been running since May 2007 at the LNGS laboratory in Italy with the primary goal of detecting solar neutrinos. The detector, a large, unsegmented liquid scintillator calorimeter characterized by unprecedented low levels of intrinsic radioactivity, is optimized for the study of the lower energy part of the spectrum. During the Phase-I (2007Phase-I ( -2010), Borexino first detected and then precisely measured the flux of the 7 Be solar neutrinos, ruled out any significant day-night asymmetry of their interaction rate, made the first direct observation of the pep neutrinos, and set the tightest upper limit on the flux of CNO solar neutrinos. In this paper we discuss the signal signature and provide a comprehensive description of the backgrounds, quantify their event rates, describe the methods for their identification, selection or subtraction, and describe data analysis. Key features are an extensive in situ calibration program using radioactive sources, the detailed modeling of the detector response, the ability to define an innermost fiducial volume with extremely low background via software cuts, and the excellent pulse-shape discrimination capability of the scintillator that allows particle identification. We report a measurement of the annual modulation of the 7 Be neutrino interaction rate. The period, the amplitude, and the phase of the observed modulation are consistent with the solar origin of these events, and the absence of their annual modulation is rejected with higher than 99% C.L. The physics implications of Phase-I results in the context of the neutrino oscillation physics and solar models are presented.

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Section: The Pep and Cno Neutrino Interaction Ratesmentioning

confidence: 99%

Final results of Borexino Phase-I on low-energy solar neutrino spectroscopy

Bellini¹,

Benziger²,

Bick³

et al. 2014

Phys. Rev. D

289

345

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“…In contrast to previous codes [9,12,13], EMILIA allows for the binding energy of photoelectrons and the rearrangement processes within the shell of scintillator atoms after the emission of such an electron. In the following, this improved model for the interaction of low-energy X-rays with the scintillation cocktail will be called the "photoelectric correction".…”

Section: Ciemat/nist Calculationsmentioning

confidence: 93%

“…In the work reported on here, the counting efficiencies were calculated by means of the KLM and KL 1 L 2 L 3 M atomic rearrangement models using the EMILIA code [8], which is a considerably enhanced version of the EMI program [9]. The EMILIA code includes a more realistic model for the interaction of photons with the scintillation cocktail via the photoelectric effect.…”

Section: Introductionmentioning

confidence: 99%

Activity standardization of 41Ca by means of liquid scintillation counting

Kossert¹,

Jörg

Gostomski

2009

Radiochimica Acta

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Liquid scintillation counting according to the CIEMAT/NIST method was used for the activity standardization of 41 Ca. The counting efficiencies were computed with two different atomic rearrangement models (KLM and KL 1 L 2 L 3 M) applying an improved model for the interaction of low-energy X-rays with the scintillation cocktail. This report comprises a detailed description of the determination of nuclear and atomic input data, sample preparation as well as a comprehensive uncertainty analysis.

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“…This method bases the computation of the counting efficiency on the simulation of the electron emission spectrum. Several simple deterministic models, which are based on averaged values for the atomic L-, M-and N-subshells, Klm (Grau Carles et al 1994), Kl 1 l 2 l 3 m (Grau Malonda 1999) and Klmn (Galiano Casas 1995), have been proposed with successful results for low-Z Auger electron emitters (Kossert & Grau Carles 2006). However, recent experiments have confirmed that those models are not sufficiently accurate for radionuclides of Z 4 30 (Grau .…”

Section: Introductionmentioning

confidence: 95%