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001     890235
005     20250813203210.0
024 7 _ |a 10.1088/1742-6596/1342/1/012105
|2 doi
024 7 _ |a Bagdasarian:2020iwh
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024 7 _ |a inspire:1776454
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024 7 _ |a 1742-6588
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024 7 _ |a 1742-6596
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024 7 _ |a 2128/27061
|2 Handle
024 7 _ |a altmetric:75769787
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024 7 _ |a WOS:001432953400105
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037 _ _ |a FZJ-2021-00822
082 _ _ |a 530
100 1 _ |a Bagdasarian, Zara
|0 P:(DE-Juel1)156420
|b 0
111 2 _ |a 15th International Conference on Topics in Astroparticle and Underground Physics
|g TAUP 2017
|c Sudbury
|d 2017-07-24 - 2017-07-28
|w Canada
245 _ _ |a Analytical response function for the Borexino solar neutrino analysis
260 _ _ |a Bristol
|c 2020
|b IOP Publ.87703
264 _ 1 |3 print
|2 Crossref
|b IOP Publishing
|c 2020-01-01
264 _ 1 |3 print
|2 Crossref
|b IOP Publishing
|c 2020-01-01
300 _ _ |a 5
336 7 _ |a CONFERENCE_PAPER
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336 7 _ |a Conference Paper
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336 7 _ |a Journal Article
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336 7 _ |a INPROCEEDINGS
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520 _ _ |a Borexino experiment is located at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, and its primary goal is detecting solar neutrinos, in particular those below 2 MeV, with unprecedentedly high sensitivity. Its technical distinctive feature is the ultra-low radioactive background of the inner scintillating core, which is the basis of the outstanding achievements obtained by the experiment (fluxes of 7Be, pep, pp, and limit on CNO). A spectral fit in the whole energy range from 200 keV up to 2 MeV has been performed for the first time, allowing to obtain simultaneously fluxes of all the solar neutrino components. To make such a fit possible, one requires the exact shapes of neutrino signals and backgrounds, as seen in the detector. Therefore, the transformation of the spectra from the original energy scale to the scale of the desired energy estimator, such as the number of hit PMTs or photoelectrons, is one of the key steps of the analysis. This conversion accounts for the energy scale non-linearity and the detector’s energy response, and can be performed using two approaches: the Monte Carlo simulation and the use of analytical models. The details and advantages of the analytical approach are presented in this contribution.
536 _ _ |a 612 - Cosmic Matter in the Laboratory (POF3-612)
|0 G:(DE-HGF)POF3-612
|c POF3-612
|f POF III
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542 _ _ |i 2020-01-01
|2 Crossref
|u http://creativecommons.org/licenses/by/3.0/
542 _ _ |i 2020-01-01
|2 Crossref
|u https://iopscience.iop.org/info/page/text-and-data-mining
588 _ _ |a Dataset connected to CrossRef, INSPIRE
650 _ 7 |a talk: Sudbury 2017/07/24
|2 INSPIRE
650 _ 7 |a neutrino: solar
|2 INSPIRE
650 _ 7 |a background: radioactivity
|2 INSPIRE
650 _ 7 |a Gran Sasso
|2 INSPIRE
650 _ 7 |a Borexino
|2 INSPIRE
650 _ 7 |a scintillation counter
|2 INSPIRE
650 _ 7 |a photomultiplier
|2 INSPIRE
650 _ 7 |a photoelectron
|2 INSPIRE
650 _ 7 |a sensitivity
|2 INSPIRE
650 _ 7 |a numerical calculations: Monte Carlo
|2 INSPIRE
650 _ 7 |a estimator
|2 INSPIRE
650 _ 7 |a spectral
|2 INSPIRE
650 _ 7 |a statistical analysis
|2 INSPIRE
650 _ 7 |a data analysis method
|2 INSPIRE
700 1 _ |a Ding, X.
|0 P:(DE-HGF)0
|b 1
700 1 _ |a Vishneva, A.
|0 P:(DE-HGF)0
|b 2
700 1 _ |a BOREXINO Collaboration
|0 P:(DE-HGF)0
|b 3
773 1 8 |a 10.1088/1742-6596/1342/1/012105
|b IOP Publishing
|d 2020-01-01
|n 1
|p 012105
|3 journal-article
|2 Crossref
|t Journal of Physics: Conference Series
|v 1342
|y 2020
|x 1742-6588
773 _ _ |a 10.1088/1742-6596/1342/1/012105
|g Vol. 1342, no. 1, p. 012105 -
|0 PERI:(DE-600)2166409-2
|n 1
|p 012105
|t Journal of physics / Conference Series
|v 1342
|y 2020
|x 1742-6588
856 4 _ |u https://juser.fz-juelich.de/record/890235/files/Bagdasarian_2020_J._Phys.%20_Conf._Ser._1342_012105.pdf
|y OpenAccess
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910 1 _ |a Forschungszentrum Jülich
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913 1 _ |a DE-HGF
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914 1 _ |y 2020
915 _ _ |a Creative Commons Attribution CC BY 3.0
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999 C 5 |a 10.1016/j.nima.2008.11.076
|9 -- missing cx lookup --
|1 Alimonti
|p 568 -
|2 Crossref
|t Nuclear Instruments and Methods A.
|v 600
|y 2009
999 C 5 |1 Agostini
|y 2017
|2 Crossref
|o Agostini 2017
999 C 5 |1 Marcocci
|y 2017
|2 Crossref
|o Marcocci 2017
999 C 5 |a 10.1016/j.nima.2008.07.139
|9 -- missing cx lookup --
|1 Smirnov
|p 410 -
|2 Crossref
|t Nucl. Inst. Meth. in Physics Research Section A.
|v 595
|y 2008
999 C 5 |a 10.1103/PhysRevD.89.112007
|1 Bellini
|9 -- missing cx lookup --
|2 Crossref
|t Physical Review D
|v 89
|y 2014

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