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@INPROCEEDINGS{Bagdasarian:890235,
      author       = {Bagdasarian, Zara and Ding, X. and Vishneva, A. and
                      {BOREXINO Collaboration}},
      title        = {{A}nalytical response function for the {B}orexino solar
                      neutrino analysis},
      journal      = {Journal of physics / Conference Series},
      volume       = {1342},
      number       = {1},
      issn         = {1742-6588},
      address      = {Bristol},
      publisher    = {IOP Publ.87703},
      reportid     = {FZJ-2021-00822},
      pages        = {012105},
      year         = {2020},
      abstract     = {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.},
      month         = {Jul},
      date          = {2017-07-24},
      organization  = {15th International Conference on
                       Topics in Astroparticle and Underground
                       Physics, Sudbury (Canada), 24 Jul 2017
                       - 28 Jul 2017},
      keywords     = {talk: Sudbury 2017/07/24 (INSPIRE) / neutrino: solar
                      (INSPIRE) / background: radioactivity (INSPIRE) / Gran Sasso
                      (INSPIRE) / Borexino (INSPIRE) / scintillation counter
                      (INSPIRE) / photomultiplier (INSPIRE) / photoelectron
                      (INSPIRE) / sensitivity (INSPIRE) / numerical calculations:
                      Monte Carlo (INSPIRE) / estimator (INSPIRE) / spectral
                      (INSPIRE) / statistical analysis (INSPIRE) / data analysis
                      method (INSPIRE)},
      cin          = {IKP-2},
      ddc          = {530},
      cid          = {I:(DE-Juel1)IKP-2-20111104},
      pnm          = {612 - Cosmic Matter in the Laboratory (POF3-612)},
      pid          = {G:(DE-HGF)POF3-612},
      typ          = {PUB:(DE-HGF)16 / PUB:(DE-HGF)8},
      UT           = {WOS:001432953400105},
      doi          = {10.1088/1742-6596/1342/1/012105},
      url          = {https://juser.fz-juelich.de/record/890235},
}