4 Conferences false [["minutes", "Minutes"], ["1", "More information about the venue"], ["notes", "Notes"], ["paper", "Paper"], ["poster", "Poster"], ["slides", "Slides"], ["summary", "Summary"]] ICN-UNAM 1482bc95ee34f0461176da21871284c8 3 icrc2007@icrc2007.unam.mx The 30th International Cosmic Ray Conference will be held from July 3, 2007 to July 11, 2007 in Merida, Yucatan, Mexico. True Merida, Mexico

2007-07-03T08:00:00 2007-07-11T19:00:00 2005-09-26T05:04:53 2024-04-12T17:46:55 Mexico/General IGeof-UNAM 40af9343b8bb9d18708b4f0252d5f53c 1107 false [["minutes", "Minutes"], ["1", "More information about the venue"], ["notes", "Notes"], ["paper", "Paper"], ["poster", "Poster"], ["slides", "Slides"], ["summary", "Summary"]] 068 (4A) HE.2.3 1 Poster UW Madison, USA 2964f01d628aa221ddcf2be5d633f569 UW Madison, USA 2964f01d628aa221ddcf2be5d633f569 UW Madison, USA 3584c5491035e86b5dbb46d699e7d811 Chiba University, Japan 40723e0e599b081036cb2acf232fc15b UW Madison, USA c2b19f5800c042db290a636f7787a766 UW Madison, USA 44d58e42b25059a01f275484b7f6a33f Merida, Mexico

Regency (Hyatt) 2007-07-09T14:45:00 2007-07-09T14:45:00 Extremely high energy (EHE) cosmic rays are expected to interact with cosmic microwave photons and generate EHE neutrinos (>10PeV). The IceCube telescope can detect the EHE neutrinos due to its large effective volume, although the expected flux is much lower than the huge flux of atmospheric background muons at lower energies. Therefore, reconstruction of the track geometry and especially the energy are essential for the EHE neutrino detection. An EHE neutrino may interact with the ice in or near IceCube and induce a muon/tau track with secondaries. The subsequent energy loss is roughly proportional to the energy of the muon/tau, so from the measured energy loss one may infer a lower limit on the energy of the parent neutrino. We are developing an event reconstruction algorithm for the track geometry and the deposited energy by using all information about the emitted Cherenkov light as detected and recorded by the IceCube digital optical modules, using waveforms. The detector response such as electronic noise, signal spreading and saturation, and also detailed information about the propagation of Cherenkov light in ice are taken into account. We will present the resolution of the event geometry and the energy obtained with this method. paper doc http://indico.nucleares.unam.mx/images/word.png word file ppt http://indico.nucleares.unam.mx/images/powerpoint.png powerpoint file pdf http://indico.nucleares.unam.mx/images/pdf_small.png pdf file odt http://indico.nucleares.unam.mx/images/writer.png writer file odp http://indico.nucleares.unam.mx/images/impress.png presentation file ods http://indico.nucleares.unam.mx/images/calc.png spreadsheet file other http://indico.nucleares.unam.mx/images/file_small.png unknown type file link http://indico.nucleares.unam.mx/images/link.png link 1 http://www.icrc2007.unam.mx/ link http://www.icrc2007.unam.mx/ doc http://indico.nucleares.unam.mx/images/word.png word file ppt http://indico.nucleares.unam.mx/images/powerpoint.png powerpoint file pdf http://indico.nucleares.unam.mx/images/pdf_small.png pdf file odt http://indico.nucleares.unam.mx/images/writer.png writer file odp http://indico.nucleares.unam.mx/images/impress.png presentation file ods http://indico.nucleares.unam.mx/images/calc.png spreadsheet file other http://indico.nucleares.unam.mx/images/file_small.png unknown type file link http://indico.nucleares.unam.mx/images/link.png link