BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Matter Effects for Ultrahigh Energy Neutrinos Detection in a Medit erranean Telescope DTSTART;VALUE=DATE-TIME:20070705T153000Z DTEND;VALUE=DATE-TIME:20070705T154200Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-4@cern.ch DESCRIPTION:Speakers: Dr. PISANTI\, Ofelia (Dipartimento di Scienze Fisich e - Università di Napoli "Federico II")\nWe perform a study of the ultra high energy neutrino detection performances of \na km^3 Neutrino Telescope sitting at the three proposed sites for ANTARES\, \nNEMO and NESTOR in th e Mediterranean sea. We focus on the effect of the \nunderwater surface pr ofile on the total amount of yearly expected tau and mu \ncrossing the fid ucial volume in the limit of full detection efficiency and energy \nresolu tion. We also emphasize the possible enhancement of matter effect by a \ns uitable choice of the geometry of the Telescope.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/51/contribution/4 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/4 END:VEVENT BEGIN:VEVENT SUMMARY:The NEMO Status Report DTSTART;VALUE=DATE-TIME:20070705T154200Z DTEND;VALUE=DATE-TIME:20070705T155400Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-856@cern.ch DESCRIPTION:Speakers: Prof. TAIUTI\, MAURO (UNIVERSITY OF GENOVA and INFN) \nThe NEMO (NEutrino Mediterranean Observatory) Project aims at the constr uction of a\nkm3-scale neutrino telescope in the Mediterranean Sea.\nAfter extensive deep-sea surveys performed in several sites in the Mediterranea n\, an\noptimal installation site for the apparatus has been identified at a depth of 3500 m\,\nabout 80 km off Capo Passero\, at the SE corner of S icily\, Italy.\nIn this talk\, we will illustrate the apparatus design and discuss its simulated\ncapabilities. We will then show the results of our long- lasting R&D efforts toward\nthe construction of the apparatus. \nSp ecifically the NEMO Project has recently completed the Phase 1\, consistin g in the\nconstruction\, deployment and operation of a subsystem which inc ludes all the key\nelements of the apparatus at a test site located at a d epth of 2000 m\, about 25 km\noff the coast of Catania. The system is pres ently fully operating and results will be\npresented in this talk. The col laboration activity is now dedicated to the\ninstrumentation of the Capo P assero site including the deployment by the end of 2007\nof a 100 km elect ro-optical cable connecting the site to the Porto Palo shore station\nand in 2008 the deployment of a full-size tower.\n\nhttps://indico.nucleares.u nam.mx/event/4/session/51/contribution/856 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/856 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Supernova Neutrino Burst at Super-Kamiokande DTSTART;VALUE=DATE-TIME:20070705T155400Z DTEND;VALUE=DATE-TIME:20070705T160600Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-791@cern.ch DESCRIPTION:Speakers: Mr. IKEDA\, Motoyasu (Okayama University)\nA search for supernova neutrino bursts was conducted using data from the \nSuper-Ka miokande (SK) detector. SK detector is an imaging water Cherenkov \ndetect or containing 50\,000 tons of pure water with 22\,500 tons of fiducial \nv olume\, and it is sensitive to core-collapse supernova explosions\nvia obs ervation of their neutrino emissions. The expected number of events \ncom prising such a burst is about 8000 in the case of a supernova explosion at \nthe typical distance in our galaxy(10kpc)\; this large signal means tha t the \ndetection efficiency anywhere within our galaxy and well past the Magellanic \nClouds is 100%. We examined a data set corresponding to 2589 .2 live days \nwhich was taken from 31st of May\, 1996 to the 15th of July \, 2001\, and from the \n24th of December\, 2002\, to the 5th of October\, 2005. However\, there is no \nevidence of such a supernova explosion duri ng the data-taking period. The \n90% C.L. upper limit on the rate of super nova explosions out to distances of\n100 kiloparsecs is found to be 0.32 S N/year.\n\nhttps://indico.nucleares.unam.mx/event/4/session/51/contributio n/791 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/791 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Supernova Relic Neutrinos at Super-Kamiokande DTSTART;VALUE=DATE-TIME:20070705T160600Z DTEND;VALUE=DATE-TIME:20070705T161800Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-822@cern.ch DESCRIPTION:Speakers: IIDA\, Takashi (ICRR\, University of Tokyo)\nSuperno va relic neutrinos (SRN) is diffuse supernova neutrino background from \na ll past supernova. No experiments have succeeded in detecting SRN yet.\nMe asurement of SRN enable us investigate history of past supernova. For \nex ample\, the flux of SRN shows star formation rate and supernova rate in \n galaxies.\nA search for SRN was conducted using Super-Kamiokande (SK) data . SK is a \nlarge water cherenkov detecter in Kamioka\, Japan. The first d ata taking phase \nof SK (SK-I) was conducted from 1996 to 2001 using 11\, 146 inner detector \nPMTs. The second phase was from 2002 to 2005 with 5\, 182 PMTs. The third \nphase has been running since JUly 2006 with 11\,129 PMTs. The search of SRN \nwas performed using SK-I and SK-II data and flux upper limit of 1.2 /cm^2 /sec \nand 3.7 /cm^2 /sec was obtained\, respect ively. Future prospects in SK-III is \nalso discussed.\n\nhttps://indico.n ucleares.unam.mx/event/4/session/51/contribution/822 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/822 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Neutrino-Induced Cascades with AMANDA data taken in 200 0-2004 DTSTART;VALUE=DATE-TIME:20070705T161800Z DTEND;VALUE=DATE-TIME:20070705T163000Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-1124@cern.ch DESCRIPTION:Speakers: TARASOVA\, Oxana (DESY)\nThe Antarctic Muon And Neut rino Detector Array (AMANDA) is a Cherenkov\ndetector deployed in the Anta rctic ice cap at the South Pole.\nThe charged-current interaction of high- energy electron or tau neutrinos\,\nas well as neutral-current interaction s of neutrinos of any flavor\, can\nproduce isolated electromagnetic or ha dronic cascades.\nThere are several advantages associated with the cascade channel in the\nsearch for a "diffuse" flux of astrophysical neutrinos.\n The energy resolution of AMANDA allows us to distinguish\nbetween a hard a strophysical spectrum and a soft atmospheric spectrum.\nIn addition\, the flux of atmospheric electron neutrinos is lower by an\norder of magnitude relative to atmospheric muon neutrinos\, while the\nbackground from downwa rd-going atmospheric muons can be suppressed due\nto their track-like topo logy.\nThe low background in this channel allows us to attain $4\\pi$\nacc eptance above energies of ~50 TeV.\nWe present the analysis of AMANDA data collected during 2000-2004.\nCompared to our previous analysis\, this dat a\nset is a factor of five larger\, resulting in a correspondingly improve d\nsensitivity for the flux of astrophysical neutrinos.\n\nhttps://indico. nucleares.unam.mx/event/4/session/51/contribution/1124 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1124 END:VEVENT BEGIN:VEVENT SUMMARY:Multi-Year Search for Ultra-High Energy Neutrinos with AMANDA-II DTSTART;VALUE=DATE-TIME:20070705T163000Z DTEND;VALUE=DATE-TIME:20070705T164200Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-1062@cern.ch DESCRIPTION:Speakers: GERHARDT\, Lisa (University of California\, Irvine)\ nAMANDA is a high volume neutrino telescope designed to search in the down -going direction for muons from \nastrophysical muon-neutrinos. It is poss ible to extend the range of AMANDA to search for neutrinos with \nextremel y high energies. The atmospheric neutrino flux becomes negligible above 10 ^15 eV\, so this value serves \nas rough energy threshold for this search. Above 10^16 eV the Earth is essentially opaque to neutrinos. This\, \ncom bined with the limited overburden above AMANDA (roughly 1.5 km)\, means th at ultra-high energy neutrinos \nwill be concentrated at the horizon. The background for this analysis consists of bundles of downgoing\, high \nene rgy muons from the the decay of cosmic rays in the atmosphere. These bundl es can be spread over areas as \nlarge as one third of the AMANDA array. S eparation of signal from the background takes advantage of the fact \nthat events from these bundles of muons have a lower light density than events from a single ultra-high \nenergy muon. Using this as well as the diffe rences in geometrical acceptance and hit topology it is possible to \nsepa rate signal from background. Three years of data from 2000 - 2002 have bee n searched and\nthe results will be presented. Methodology and results for a new search using 2003 data will also be presented.\n\nhttps://indico.nu cleares.unam.mx/event/4/session/51/contribution/1062 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1062 END:VEVENT BEGIN:VEVENT SUMMARY:Optimized neutrino point source search strategies for AMANDA and r esults from 2005 DTSTART;VALUE=DATE-TIME:20070705T164200Z DTEND;VALUE=DATE-TIME:20070705T165400Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-1-1090@cern.ch DESCRIPTION:Speakers: Mr. BRAUN\, James (University of Wisconsin - Madison )\nCurrent point source searches mostly apply only the direction of the re constructed\nevent\; furthermore\, they reduce available information by gr ouping events into sky\nbins. In this analysis we use a search based on ma ximum likelihood techniques\,\nutilizing both event direction and energy\, to enhance our ability to detect point\nsources. Especially\, use of ener gy information allows us to fit the spectral index of\na hypothetical sour ce along with flux. This method improves both sensitivity and\ndiscovery p otential of the AMANDA-II array significantly. The method can naturally be \napplied to IceCube and allows superposition of data from detectors with different\nsensitivity and angular resolution\, such as the IceCube array which changes and\nimproves with each season of construction.\n\nhttps://i ndico.nucleares.unam.mx/event/4/session/51/contribution/1090 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1090 END:VEVENT BEGIN:VEVENT SUMMARY:The ANTARES Neutrino Telescope: status report DTSTART;VALUE=DATE-TIME:20070705T132900Z DTEND;VALUE=DATE-TIME:20070705T134100Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-0-89@cern.ch DESCRIPTION:Speakers: Dr. KOUCHNER\, Antoine (Laboratoire APC)\nANTARES is a large volume\, deep-sea\, neutrino telescope currently under constructi on off La Seyne-sur-mer\, \nFrance. \nNeutrino telescopes aims at detectin g neutrinos as a new probe for a sky study at energies greater than 1 TeV. \nThe detection principle relies on the observation\, using photomultipli ers\, of the Cherenkov light emitted by \ncharged leptons induced by neutr ino interactions in the surrounding detector medium.\nSince January 2007\, the ANTARES detector consists of 5 lines\, comprising 75 optical detector s each\, connected to \nthe shore via an undersea cable from the site at a depth of 2475m. The data from these lines not only allow an \nextensive s tudy of the detector properties but also the reconstruction of downward go ing cosmic ray muons and \nthe search for the first upward going neutrino induced muons.\nThe operation of these lines follows on from that of the A NTARES instrumentation line\, which has provided data \nfor more than a ye ar on the detector stability and the environmental conditions. \nThe full 12 line detector is planned to be fully operational in January 2008.\n\nht tps://indico.nucleares.unam.mx/event/4/session/51/contribution/89 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/89 END:VEVENT BEGIN:VEVENT SUMMARY:The ANTARES detector: background sources and effects on detector p erformance DTSTART;VALUE=DATE-TIME:20070705T134100Z DTEND;VALUE=DATE-TIME:20070705T135300Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-0-547@cern.ch DESCRIPTION:Speakers: Dr. ESCOFFIER\, Stephanie (CNRS/IN2P3/CPPM)\nThe ANT ARES Collaboration is deploying a large neutrino detector at a depth of 25 00 m\nin the Mediterranean Sea\, 40 km off shore from La Seyne-sur-Mer in South France. The\nconstruction of this 12-line detector with 75 phototube s per line will be completed\nby the end of 2007. Data taking has begun si nce April 2005 with an instrumentation\nline also equipped with optical mo dules. The first 5 detector lines are operational\nsince January 2007. The telescope is aimed to observe high energy cosmic neutrinos\nthrough the d etection of the Cerenkov light produced by up-going induced muons.\nBackgr ound sources are due to atmospheric neutrinos as well as misreconstructed\ natmospheric muons. Additional backgrounds inherent to the sea water envir onment come\nfrom 40K decay and marine organisms luminescence. While the c ontribution of the\nformer is expected to be constant at a level of about 45 kHz\, the bioluminescence has\nshown large time variations\, with perio ds of very high activity\, up to several\nhundred kHz. Description of thes e background sources will be reported\, and effects on\ndetector performan ce will be described. Methods recently developed to improve the\ndetectio n efficiency in high background periods will be described\, together with some\nof the results obtained.\n\nhttps://indico.nucleares.unam.mx/event/4 /session/51/contribution/547 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/547 END:VEVENT BEGIN:VEVENT SUMMARY:Expected discovery potential and sensitivity to neutrino\npoint-li ke sources of the ANTARES neutrino telescope. DTSTART;VALUE=DATE-TIME:20070705T135300Z DTEND;VALUE=DATE-TIME:20070705T140500Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-0-638@cern.ch DESCRIPTION:Speakers: Mr. AGUILAR SÁNCHEZ\, Juan Antonio (IFIC)\nThe ANTA RES telescope is being built in the Mediterranean Sea. The detector\nconsi sts of a 3D array of photomultipliers (PMTs) that detects the Cherenkov\nl ight induced by the muons produced in neutrino interactions. Since the\nne utrino fluxes from point-like sources are expected to be small\, it is of\ nthe utmost importance to take advantage of the ANTARES accurate pointing\ npower (angular resolution less than 0.3 degrees for muon events above 10 TeV)\nto disentangle a possible signal from the unavoidable atmospheric ne utrino\nbackground. In order to distinguish an excess of neutrino events f rom the\nbackground\, several searching algorithms have been developed wit hin the\nANTARES collaboration. In this contribution\, the discovery poten tial and\nsensitivity to point-like sources of the ANTARES neutrino telesc ope are\npresented comparing the results from different algorithms.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/51/contribution/638 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/638 END:VEVENT BEGIN:VEVENT SUMMARY:Diffuse high-energy neutrino searches in AMANDA-II and IceCube: re sults and future prospects DTSTART;VALUE=DATE-TIME:20070705T143500Z DTEND;VALUE=DATE-TIME:20070705T144700Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-3-1103@cern.ch DESCRIPTION:Speakers: HILL\, Gary (University of Wisconsin\, Madison)\, HO DGES\, Jessica (University of Wisconsin\, Madison)\, HOSHINA\, Kotoyo (Uni versity of Wisconsin\, Madison)\nThe AMANDA-II data collected during the p eriod 2000-03 have been analysed in a search \nfor a diffuse flux of high- energy extra-terrestrial neutrinos from the sum of all sources in \nthe un iverse. With no excess of events seen\, an upper limit on an E-2 flux of E 2 Phi < 8.8 \nx 10-8 GeV cm-2 s-1 sr-1 was obtained. The astrophysical imp lications of this bound and \nof others obtained for specific models will be discussed. The first results from analysis of \nthe IceCube 9 string de tector and prospects for the current 22 string detector will be \npresente d.\n\nhttps://indico.nucleares.unam.mx/event/4/session/51/contribution/110 3 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1103 END:VEVENT BEGIN:VEVENT SUMMARY:One Year IceCube Point Source Analysis DTSTART;VALUE=DATE-TIME:20070705T144700Z DTEND;VALUE=DATE-TIME:20070705T145900Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-3-764@cern.ch DESCRIPTION:Speakers: Dr. FINLEY\, Chad (University of Wisconsin\, Madison )\nThe construction of the IceCube Neutrino Observatory began during the a ustral summer\nof 2004-05\, and is expected to continue through 2011. Duri ng 2006\, nine of the\nprojected 80 strings were already deployed and taki ng data\, making IceCube an\noperational neutrino observatory while still at about 10% of its final size. We\npresent the first results of a point-s ource search based on the analysis of this year\nof data. We also characte rize the angular resolution\, effective area\, and sensitivity\nto point s ources of the nine-string detector configuration\, and discuss how the\npe rformance is expected to improve as the detector moves toward completion.\ n\nhttps://indico.nucleares.unam.mx/event/4/session/51/contribution/764 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/764 END:VEVENT BEGIN:VEVENT SUMMARY:The first results on the search for extremely high energy neutrino s by the IceCube detector DTSTART;VALUE=DATE-TIME:20070705T170200Z DTEND;VALUE=DATE-TIME:20070705T171300Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-275@cern.ch DESCRIPTION:Speakers: Dr. ISHIHARA\, Aya (Chiba University)\nExtremely hig h energy (EHE) cosmic neutrinos (E>10^8GeV) are considered to carry\nimpor tant information about particle acceleration mechanisms in the universe an d the\norigin of EHE cosmic-ray. The IceCube experiment is uniquely design ed to detect\nhighly energetic astrophysical neutrino events using Antarct ic ice as a natural\nCherenkov radiator to overcome difficulties associate d in the search \nfor EHE neutrino. We study event samples recorded durin g 2006 by IceCube's deep\nin-ice 540 optical sensors tied to 9 electric ca bles and 68 sensors at the South Pole\nice surface. In the EHE region\, b ecause of the increase of the neutrino\ncross-section with energy\, mean f ree path of neutrino becomes shorter than the Earth\nradius\, and secondar y charged particles created during the neutrino propagation are\nnot the m inimum ionizing particle but they loose energy by stochastic radiative\npr ocess\, which implies that EHE neutrino events reach to the IceCube detect or are\nfrom horizon or above leaving luminous bulk of Cherenkov photons. We show that these\nEHE signatures are distinguished from background atmos pheric (bundled) muons using a\ndetailed Monte Carlo simulation compared t o real data samples. Finally the most\nupdated results of EHE neutrino sea rch on 2006 IceCube data are presented in energy\nregime greater than 10^8 GeV.\n\nhttps://indico.nucleares.unam.mx/event/4/session/51/contribution/ 275 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/275 END:VEVENT BEGIN:VEVENT SUMMARY:Limits to the diffuse flux of UHE neutrinos at EeV energies from t he Pierre Auger Observatory DTSTART;VALUE=DATE-TIME:20070705T171300Z DTEND;VALUE=DATE-TIME:20070705T172400Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-603@cern.ch DESCRIPTION:Speakers: Dr. BLANCH-BIGAS\, Oscar (LPNHE)\nThe Pierre Auger O bservatory has the capability of detecting\nultra-high energy neutrinos by searching for very inclined showers\nwith a significant electromagnetic c omponent. In this work we discuss\nthe discrimination power of the instrum ent for ultra-high energy\nneutrinos. Based on the data collected since J anuary 2004 an upper\nlimit to the diffuse flux of neutrinos at EeV energi es is presented\nand systematic uncertainties are discussed.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/51/contribution/603 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/603 END:VEVENT BEGIN:VEVENT SUMMARY:An upper limit on the upward-going electron-neutrino flux from the HiRes instrument DTSTART;VALUE=DATE-TIME:20070705T172400Z DTEND;VALUE=DATE-TIME:20070705T173500Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-708@cern.ch DESCRIPTION:Speakers: Dr. SCOTT\, Lauren (Rutgers University\, USA)\nAir-f luorescence detectors such as the High Resolution Fly's Eye (HiRes) instru ment\nare very sensitive to upward-going\, Earth-skimming ultrahigh energy \nelectron-neutrino-induced showers.\nThis is due to the relatively large interaction cross sections of these high-energy\nneutrinos and the Landau- Pomeranchuk-Migdal (LPM) effect\, which is responsible for a\nsignificant decrease in the cross sections for bremsstrahlung and pair production\,\nr endering charged-current\nelectron-neutrino-induced showers occurring deep in the Earth's crust detectable as\nthey exit the Earth into the atmosphe re. The search for upward-going\nneutrino-induced showers in the entire H iRes-II monocular dataset has yielded a null\nresult. From a full LPM cal culation of the energy spectrum of charged particles as a\nfunction of pri mary energy and depth for electron-induced showers in rock\, we\ncalculate the resulting profile of these showers in air.\nA full detector Monte Car lo simulation to determine the detector response to\nupward-going electron -neutrino-induced cascades is described and an upper limit on\nthe flux of electron-neutrinos is given.\n\nhttps://indico.nucleares.unam.mx/event/4/ session/51/contribution/708 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/708 END:VEVENT BEGIN:VEVENT SUMMARY:Diffuse Astrophysical Neutrino Flux Limit from Super-Kamiokande us ing Ultra-High Energy Upward-Going Muons DTSTART;VALUE=DATE-TIME:20070705T173500Z DTEND;VALUE=DATE-TIME:20070705T174600Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-595@cern.ch DESCRIPTION:Speakers: SWANSON\, Molly (Massachusetts Institute of Technolo gy)\nMany astrophysical models predict a diffuse flux of high-energy neutr inos from active\ngalactic nuclei and other extra-galactic sources. At muo n energies above 1 TeV\, the\nupward-going muon flux induced by neutrinos from active galactic nuclei is expected\nto exceed the flux due to atmosph eric neutrinos. We have performed a search for this\nastrophysical neutrin o flux by looking for upward-going muons in the highest energy\ndata sampl e from the Super-Kamiokande detector using 1679.6 live days of data. We\nf ound one extremely high energy upward-going muon event\, compared with an expected\natmospheric neutrino background of 0.46 plus or minus 0.23 event s. Using this result\,\nwe set an upper limit on the diffuse flux of upwar d-going muons due to neutrinos from\nastrophysical sources in the muon ene rgy range 3.16-100 TeV.\n\nhttps://indico.nucleares.unam.mx/event/4/sessio n/51/contribution/595 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/595 END:VEVENT BEGIN:VEVENT SUMMARY:A search for neutrino bursts from gravitational collapse of stars at Baksan Underground Scintillation Telescope. DTSTART;VALUE=DATE-TIME:20070705T174600Z DTEND;VALUE=DATE-TIME:20070705T175700Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-442@cern.ch DESCRIPTION:Speakers: Dr. NOVOSELTSEV\, Yuriy (Institute for Nuclear Resea rch of RAS)\nCurrent status and results of the experiment on recording\nne utrino bursts are presented.\nThe observation livetime (since 1980) is 22. 6 years.\nThe upper bound of collapse frequency in our Galaxy \nis 0.10 $y ^{-1}$ (90% CL).\n\nhttps://indico.nucleares.unam.mx/event/4/session/51/co ntribution/442 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/442 END:VEVENT BEGIN:VEVENT SUMMARY:Simulation of Double-Bang Events in the Atmosphere DTSTART;VALUE=DATE-TIME:20070705T175700Z DTEND;VALUE=DATE-TIME:20070705T180800Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-754@cern.ch DESCRIPTION:Speakers: Dr. ADREGA DE MOURA\, Celio (Departamento de Fisica\ , Cinvestav - IPN)\nWe use CORSIKA+Herwig simulation code to produce ultra -high energy neutrino\ninteractions in the atmosphere. Our aim is to repro duce extensive air showers\noriginated by extragalactic tau-neutrinos. As we have no code available which can\nsimulate the tau-neutrino as primary particle in the atmosphere\, we use muon-neutrino\nas primaries. For charg ed current tau-neutrino interactions in the atmosphere\, it is\nexpected t hat a tau is produced and may decay before reaching the ground. That\nphen omenon makes possible the generation and detection of two extensive air sh owers\,\nthe so called Double-Bang events. We simulate the tau decay using interactions of\npions in the atmosphere. In spite of those two approxima tions\, muon-neutrino first\ninteraction instead of tau-neutrino and pion interaction instead of the tau decay\, we\ncan make a quantitative analysi s of the main characteristics of the Double-Bang\nevents that may be obser ved in the atmosphere with ultra-high energy cosmic ray\nobservatories.\n\ nhttps://indico.nucleares.unam.mx/event/4/session/51/contribution/754 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/754 END:VEVENT BEGIN:VEVENT SUMMARY:GRB neutrino detection via time profile stacking. DTSTART;VALUE=DATE-TIME:20070705T180800Z DTEND;VALUE=DATE-TIME:20070705T181900Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-267@cern.ch DESCRIPTION:Speakers: Dr. VAN EIJNDHOVEN\, Nick (Utrecht University)\nA me thod is presented for the identification of high-energy neutrinos from\nga mma ray bursts by means of a large-scale neutrino telescope.\nThe procedur e makes use of a time profile stacking technique of observed \nneutrino in duced signals in correlation with satellite observations.\nBy selecting a rather wide time window\, a possible difference between the \narrival time s of the gamma and neutrino signals may also be identified. \nThis might p rovide insight in the particle production processes at the source.\nBy mea ns of a toy model it will be demonstrated that a statistically significant \nsignal can be obtained with a cubic km scale neutrino telescope on a sam ple\nof 500 gamma ray bursts for a signal rate as low as 1 detectable neut rino\nfor 3% of the bursts.\n\nhttps://indico.nucleares.unam.mx/event/4/se ssion/51/contribution/267 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/267 END:VEVENT BEGIN:VEVENT SUMMARY:Search for neutrino bursts from gravitational stellar collapses wi th LVD: update to 2007 DTSTART;VALUE=DATE-TIME:20070705T181900Z DTEND;VALUE=DATE-TIME:20070705T183000Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-2-1022@cern.ch DESCRIPTION:Speakers: THE LVD COLLABORATION\, - (LNGS-INFN)\nThe Large Vol ume Detector LVD (Gran Sasso National Laboratory\, Italy) is a neutrino sc intillator observatory \nmonitoring the Galaxy since 1992\, searching for low energy neutrino bursts from gravitational stellar \ncollapses. We pres ent the status of the detector that reached its final active mass of 1000 t in 2001. No \ncandidates have been detected over all the fifteen years o f observation: the resulting 90% c.l. upper limit to \nthe rate of gravita tional stellar collapses in the Galaxy will be presented.\n\nhttps://indic o.nucleares.unam.mx/event/4/session/51/contribution/1022 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1022 END:VEVENT BEGIN:VEVENT SUMMARY:ANITA: First Flight Overview and Detector Performance DTSTART;VALUE=DATE-TIME:20070707T164500Z DTEND;VALUE=DATE-TIME:20070707T165700Z DTSTAMP;VALUE=DATE-TIME:20261012T221524Z UID:indico-contribution-51-4-1095@cern.ch DESCRIPTION:Speakers: PALLADINO\, Kimberly J. (Dept. of Physics\, The Ohio State University Columbus\, OH 43210)\nThe ANtarctic Impulsive Transient Antenna (ANITA) searches for\nultra high energy neutrinos interacting in t he antarctic ice cap.\nIt is a long duration balloon experiment composed o f an array of\nbroadband dual-polarized horn antennas that had its first s cience\nflight over Antarctica in December 2006 through January 2007. ANIT A\nrelies upon the Askaryan effect\, in which a particle shower\nin a dens e medium emits coherent Cherenkov radiation at radio wavelengths\,\nfor th e detection of a neutrino induced shower. ANITA is designed to\ndetect or constrain flux models of ultra high energy neutrinos\ncreated by the inter action of ultra high energy cosmic rays with\nthe cosmic microwave backgro und. In this paper we discuss the detector\nperformance during the first ANITA flight and look specifically to the\nRF sensitivity and the angular resolution of the instrument.\n\nhttps://indico.nucleares.unam.mx/event/4/ session/51/contribution/1095 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/51/contribution/1095 END:VEVENT END:VCALENDAR