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@TECHREPORT{Tarasova:83072,
      author       = {Tarasova, O. and Kowalski, M. and Walter, M. and DESY},
      collaboration = {{IceCube Collaboration}},
      title        = {{S}earch for {N}eutrino-{I}nduced {C}acscades with {AMANDA}
                      {D}ata {T}aken in 2000-2004},
      number       = {arXiv:0711.0353},
      address      = {Ciudad de Mexico},
      publisher    = {Universidad Nacional Autonoma de Mexico},
      reportid     = {PHPPUBDB-5455, arXiv:0711.0353},
      pages        = {83-86},
      year         = {2007},
      abstract     = {The Antarctic Muon and Neutrino Detector Array (AMANDA) is
                      a Cherenkov detector deployed in the Antarctic ice cap at
                      the South Pole. The carged-current interaction of
                      high-energy electron or tau neutrinos, as well as the
                      neutral-current interactions of neutrinos of any flavor, can
                      produce isolated electromagnetic or hadronic cascades. There
                      are several advantages associated with the cascade channel
                      in the search for a "diffuse" flux of astrophysical
                      neutrinos. The energy resolution of AMANDA allows us to
                      distinguish between a hard astrophysical spectrum and a soft
                      atmospheric spectrum. In addition, the flux of atmospheric
                      electron neutrinos is lower ba an order of magnitude
                      relative to atmospheric nuon neutrinos, while the background
                      from downward-going atmospheric muons can be suppressed due
                      to their track-like topology. The low background in this
                      channel allows us to attain 4π acceptance above energies of
                      ∼ 50 TeV. We present the analysis of AMANDA data collected
                      during 2000-2004. Compared to our previous analysis, this
                      data set is a factor of five larg er, resulting in a
                      correspondingly improved sensitivity for the flux of
                      astrophysical neutrinos.},
      month         = {Jul},
      date          = {2007-07-03},
      organization  = {30th International Cosmic Ray
                       Conference, Merida (Mexico), 3 Jul 2007
                       - 11 Jul 2007},
      cin          = {ZNP(-2012)},
      cid          = {$I:(DE-H253)ZNP_-2012_-20130307$},
      pnm          = {520 - Astroteilchenphysik (POF1-500)},
      pid          = {G:(DE-HGF)POF1-520},
      experiment   = {EXP:(DE-H253)AMANDA-20170101},
      typ          = {PUB:(DE-HGF)29 / PUB:(DE-HGF)15},
      eprint       = {0711.0353},
      howpublished = {arXiv:0711.0353},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:0711.0353;\%\%$},
      url          = {https://bib-pubdb1.desy.de/record/83072},
}