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000890238 0247_ $$2ISSN$$a1742-6588
000890238 0247_ $$2ISSN$$a1742-6596
000890238 0247_ $$2arXiv$$aarXiv:1805.11125
000890238 0247_ $$2Handle$$a2128/27070
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000890238 1001_ $$aDing, X. F.$$b0
000890238 1112_ $$a15th International Conference on Topics in Astroparticle and Underground Physics$$cSudbury$$d2017-07-24 - 2017-07-28$$gTAUP 2017$$wCanada
000890238 245__ $$aSpeeding up complex multivariate data analysis in Borexino with parallel computing based on Graphics Processing Unit
000890238 260__ $$aBristol$$bIOP Publ.87703$$c2020
000890238 264_1 $$2Crossref$$3print$$bIOP Publishing$$c2020-01-01
000890238 264_1 $$2Crossref$$3print$$bIOP Publishing$$c2020-01-01
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000890238 3367_ $$0PUB:(DE-HGF)8$$2PUB:(DE-HGF)$$aContribution to a conference proceedings$$bcontrib$$mcontrib$$s1754992079_25206
000890238 500__ $$a5 pages, 2 figures, proceeding for TAUP 2017 XV International Conference on Topics in Astroparticle and Underground Physics
000890238 520__ $$aA spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector response and pile-up effects. Moreover, the convergence time increases to more than two days when including extra computations for the discrimination of 11C and external γs. In sharp contrast, with the GPU-based fitter it takes less than 10 seconds and less than four minutes, respectively. This fitter is developed utilizing the GooFit project with customized likelihoods, pdfs and infrastructures supporting certain analysis methods. In this proceeding the design of the package, developed features and the comparison with the original CPU fitter are presented.
000890238 536__ $$0G:(DE-HGF)POF3-612$$a612 - Cosmic Matter in the Laboratory (POF3-612)$$cPOF3-612$$fPOF III$$x0
000890238 542__ $$2Crossref$$i2020-01-01$$uhttp://creativecommons.org/licenses/by/3.0/
000890238 542__ $$2Crossref$$i2020-01-01$$uhttps://iopscience.iop.org/info/page/text-and-data-mining
000890238 588__ $$aDataset connected to CrossRef, INSPIRE
000890238 650_7 $$2INSPIRE$$aneutrino: solar
000890238 650_7 $$2INSPIRE$$aBorexino
000890238 650_7 $$2INSPIRE$$aspectral
000890238 650_7 $$2INSPIRE$$agraphics
000890238 650_7 $$2INSPIRE$$apile-up
000890238 7001_ $$0A.Vishneva.2$$aVishneva, A.$$b1
000890238 7001_ $$0P:(DE-Juel1)171602$$aPenek, Ömer$$b2$$eCorresponding author
000890238 7001_ $$0S.Marcocci.1$$aMarcocci, S.$$b3
000890238 7001_ $$0P:(DE-HGF)0$$aBorexino Collaboration$$b4
000890238 77318 $$2Crossref$$3journal-article$$a10.1088/1742-6596/1342/1/012115$$bIOP Publishing$$d2020-01-01$$n1$$p012115$$tJournal of Physics: Conference Series$$v1342$$x1742-6588$$y2020
000890238 773__ $$0PERI:(DE-600)2166409-2$$a10.1088/1742-6596/1342/1/012115$$gVol. 1342, no. 1, p. 012115 -$$n1$$p012115$$tJournal of physics / Conference Series$$v1342$$x1742-6588$$y2020
000890238 8564_ $$uhttps://juser.fz-juelich.de/record/890238/files/Ding_2020_J._Phys.%20_Conf._Ser._1342_012115.pdf$$yOpenAccess
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000890238 9141_ $$y2020
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