BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Plenary Session: Conference Summary DTSTART;VALUE=DATE-TIME:20111014T143000Z DTEND;VALUE=DATE-TIME:20111014T151500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-27@cern.ch DESCRIPTION:Speakers: DE JONG\, Maarten (NIKHEF)\nhttp://indico.cern.ch/co ntributionDisplay.py?contribId=27&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=27&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The neutrino sky at very high energies DTSTART;VALUE=DATE-TIME:20111013T120000Z DTEND;VALUE=DATE-TIME:20111013T125000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-29@cern.ch DESCRIPTION:Speakers: AHLERS\, Markus ()\nNeutrino astronomy opens a new w indow for the observation and study of high-energy phenomena in our Univer se. The emission of high energy neutrinos is intimately related to that of gamma rays and cosmic rays (CRs) via hadronic interactions in extragalact ic sources or the cosmic environment. I will discuss our present expectati ons for the cosmogenic neutrino flux associated with the propagation of ul tra-high energy (UHE) CRs in the cosmic radiation background. This flux is a "guaranteed" contribution to the diffuse EeV neutrino background but sh ows a strong model dependence on the UHE CR scenario. Specific models of e xtragalactic TeV to PeV neutrino sources are already testable by large vol ume neutrino observatories like IceCube. I will show how present limits on diffuse and point-source neutrino fluxes can be used to constrain candida te sources of UHE CRs like gamma ray bursts.\n\nhttp://indico.cern.ch/cont ributionDisplay.py?contribId=29&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=29&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:IceCube results DTSTART;VALUE=DATE-TIME:20111012T083000Z DTEND;VALUE=DATE-TIME:20111012T092000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-4@cern.ch DESCRIPTION:Speakers: RESCONI\, Elisa ()\nThe construction of IceCube neut rino telescope and IceTop surface array was successfully completed at the South Pole during December\, 2010. IceCube is the most sensitive telescop e to date for observing high energy neutrino sources.\nThe performance of the IceCube detector and a selection of results will be reported from earl ier years as the detector increased in size from 40\, 59 and 79 strings. New analysis methods developed for the study of the Southern Hemisphere as well as for extended regions in the sky will be emphasized. The long ter m experience with AMANDA and IceCube has proven that the South Pole ice is an ideal\nsite for astroparticle physics. New ideas and possible future p rojects beyond IceCube will also be presented.\n\nhttp://indico.cern.ch/co ntributionDisplay.py?contribId=4&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=4&sessionId=0&c onfId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Toward precision neutrino physics with DeepCore and beyond DTSTART;VALUE=DATE-TIME:20111014T090000Z DTEND;VALUE=DATE-TIME:20111014T093000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-8@cern.ch DESCRIPTION:Speakers: DEYOUNG\, Tyce ()\nDeepCore\, the fully contained lo w energy extension to IceCube\, extends IceCube's sensitivity for indirect dark matter searches and atmospheric neutrino oscillations. With the fir st year of DeepCore data we observe a significant sample of atmospheric ne utrino-induced cascades\, confirming the scientific potential of this appr oach. We will discuss ideas for PINGU\, a further IceCube infill array wh ich aims for an energy threshold of around 1 GeV to support a precision Ic eCube neutrino physics program. In the longer term\, we are exploring the feasibility of a precision neutrino physics program with a multi-megaton\ , sub-GeV detector in the Antarctic ice cap.\n\nhttp://indico.cern.ch/cont ributionDisplay.py?contribId=8&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=8&sessionId=0&c onfId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Specification of Underwater Fiber Optic Connectors for Neutrino Te lescope systems DTSTART;VALUE=DATE-TIME:20111012T125000Z DTEND;VALUE=DATE-TIME:20111012T131500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-59@cern.ch DESCRIPTION:Speakers: THUMBECK\, Steven (Seacon Advanced Products\, LLC)\n Connectors for underwater use are an important component of many subsea sy stems\, they make it easier to conduct onshore or offshore testing\, easie r to manage cabled assemblies and facilitate ease of installation during d eployment. Underwater connectors come in a variety of types and configura tions\, a majority of the underwater connectors are either dry-mate or wet -mate having electrical or optical contacts or a combination of both\, typ ically called hybrid connectors. These underwater connectors are being us ed for Subsea Neutrino Telescope systems\, demonstrating their value to Ne utrino detection projects. Currently\, Neutrino Telescope systems are typ ically making use of the commercially available underwater connectors. Th ese commercial connectors have been developed over the past decades for na val acoustic arrays\, ocean science observatories and connection of umbili cal’s and control equipment for offshore oil and gas facilities. As the offshore industry evolves\, testing and demonstrating newer Subsea Neutri no Telescope systems\, brings more focus on critical technologies required for the system to perform reliably. While\, certain underwater connector s are well proven with a good field history and track record\, more advanc ed optically based Neutrino Telescope systems utilizing fiber optic dry-ma te and wet-mate underwater connectors become an increased focus on reliabi lity to ensure that these technologies are ready for the market.\n\nhttp:/ /indico.cern.ch/contributionDisplay.py?contribId=59&sessionId=6&confId=143 656 LOCATION:Physics Lecture Hall HF URL:http://indico.cern.ch/contributionDisplay.py?contribId=59&sessionId=6& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:KM3NeT sensitivity and discovery potential for galactic point-like sources DTSTART;VALUE=DATE-TIME:20111012T153000Z DTEND;VALUE=DATE-TIME:20111012T155000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-58@cern.ch DESCRIPTION:Speakers: Dr. SAPIENZA\, piera (lns)\nThe KM3NeT consortium ht tp://www.km3net.org aims at the construction of a cubic-kilometre-scale ne utrino telescope for the Northern hemisphere with an integrated platform f or earth and deep sea sciences. \nThe telescope location in the Mediterran ean Sea will allow for surveying a large part of the Galactic Plane (87%)\ , including the Galactic Centre\, thus complementing the sky coverage of I ceCube at the South Pole. Due to its good angular resolution\, 70% of sele cted events lie within 0.2° of the neutrino direction\, and large size\, about 5 km3 of instrumented volume\, this project will provide the scienti fic community with a very powerful instrument to study many astrophysical objects\, including supernova remnants\, active galactic nuclei\, gamma-ra y bursts and possibly also dark matter. \nOne of the main physics objectiv e of KM3NeT is the search of neutrinos from galactic sources. \nIn this co ntribution first results on sensitivity and discovery potential for point- like galactic sources and in particular for the Supernova Remnant RXJ1713 are presented. Further improvements on the reconstruction algorithm and de tector optimisation are in progress.\n\nhttp://indico.cern.ch/contribution Display.py?contribId=58&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=58&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The KM3NeT high energy neutrino telescope and Fermi bubbles: some predicitions DTSTART;VALUE=DATE-TIME:20111012T161000Z DTEND;VALUE=DATE-TIME:20111012T163000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-57@cern.ch DESCRIPTION:Speakers: Dr. CONIGLIONE\, Rosa (INFN- Laboratori Nazionali de l Sud)\nA recent analysis of the Fermi data [1] provides evidence of the e mission of high energy gamma rays (up to 100 GeV) with a high intensity E- 2 spectrum. This emission was detected as originating from two large areas around the Galactic center\, spanning 50° above and below the Galactic c enter and 40° in longitude\, with no spacial evidence of variation both i n the spectrum shape and in the intensity. Currently\, all the observed fe atures of the Fermi bubbles are not fully explained by a leptonic mechanis m and an hadronic mechanism has been proposed [2]. The possible origin of high energy gammas from an hadronic mechanism makes these bubbles promisin g sources for high energy neutrino emission.\nKM3NeT [3] is a consortium w ith the aim to develop a deep-sea research infrastructure hosting a multi- cubic-kilometer scale high energy neutrino detector in the Mediterranean s ea. The location of the detector makes possible the survey of the Galacti c center and of a large area surrounding the center and makes this future detector the ideal instrument for the observation of neutrino from Fermi b ubbles. \nIn this work some predictions\, based on Monte Carlo simulations and on the high energy gamma observations\, regarding the possible detect ion of high energy neutrino from Fermi bubbles will be presented. \n [1] M eng Su et al.\, Astroph. Journal 724 :1044-1082\, 2010\n[2] R.M. Crocker a nd F. Aharonian Phys. Rev. Lett. 106 (2011)101102 \n[3] KM3NeT web page ht tp://www.km3net.org/home.php\n\nhttp://indico.cern.ch/contributionDisplay. py?contribId=57&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=57&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Simulation Chain for Acoustic UHE Neutrino Detectors DTSTART;VALUE=DATE-TIME:20111013T083000Z DTEND;VALUE=DATE-TIME:20111013T085000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-56@cern.ch DESCRIPTION:Speakers: NEFF\, Max (ECAP)\nAcoustic neutrino detection is a promising approach for large-scale ultra high energy neutrino detectors in water. The presented simulation chain is designed within the SeaTray/IceT ray software framework. Its modular architecture is highly flexible and ma kes it easy to adapt to different detector geometries\, environmental cond itions or hardware used. The simulation chain covers the generation of the acoustic pulse produced by a neutrino interaction and the propagation to the sensors within the detector. In this phase of the development\, ambien t and transient noise models for the Mediterranean Sea and data acquisitio n hardware\, which is similar to the one used in ANTARES/AMADEUS\, are imp lemented. A pre-selection scheme for neutrino-like signals based on matche d filtering is employed\, as it can be used for on-line filtering. To simu late the whole processing chain for experimental data\, signal classificat ion and acoustic source reconstruction algorithms are integrated.\nIn the presentation an overview of the design and capabilities of the simulation chain will be given\, as well as some applications and preliminary studies .\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=56&sessionId=1 &confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=56&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Photonics-oriented data transmission network for the KM3NeT protot ype detection unit DTSTART;VALUE=DATE-TIME:20111013T092000Z DTEND;VALUE=DATE-TIME:20111013T094000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-51@cern.ch DESCRIPTION:Speakers: HOGENBIRK\, Jelle (Nikhef (for the KM3NeT consortium ))\nThe design of the readout and data acquisition system of the future KM 3NeT neutrino telescope employs 10Gbps photonic technologies for data tran smission to shore. The photonic architecture can handle standard transmiss ion protocols. The generic scheme is based on DWDM technology using lasers on shore and optical modulators in each of the 15.000 Digital Optical Mod ules (DOMs) arranged on vertical detection units anchored to the seabed. E ach DOM will house 31 small-size PMTs together with auxiliary transducers. A 100 km electrical/optical fibre cable will connect the DOMs to the stor e. The readout system will guarantee a unique optical connection between e ach DOM and the shore. A small-scale prototype of a detection unit with fo ur DOMs is now in a realization phase for a.o. in-situ testing of the data transmission network. We will present results of laboratory tests of the photonics-oriented transmission layer of the network being realised for th e prototype detection unit.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=51&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=51&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:GPUs for Parallel Trigger Implementation For Muon Detection DTSTART;VALUE=DATE-TIME:20111012T163000Z DTEND;VALUE=DATE-TIME:20111012T164500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-53@cern.ch DESCRIPTION:Speakers: Dr. BOUHADEF\, Bachir (INFN Pisa.)\nBachir BOUHADEF\ , INFN Pisa & Physics department of Pisa\, On behalf of NEMO Collaboration .\n\nGraphics Processing Units are high performance co-processors original ly intended to improve the use and quality of computer graphics applicatio ns. Because of their potential\, researchers have extended their use beyon d the computer graphics scope. The main goal of this work is to evaluate t he time benefit of using GPUs rather than CPUs for muon trigger implementa tion into the NEMO Trigger and Data Acquisition System (TriDAS). A simulat ion on a 16 plane Nemo Tower shows a possibility of reduced time requireme nts\, in addition to power consumption and hardware space benefits.\n\nhtt p://indico.cern.ch/contributionDisplay.py?contribId=53&sessionId=8&confId= 143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=53&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A TDC for characterization of KM3NeT PMTs DTSTART;VALUE=DATE-TIME:20111012T163000Z DTEND;VALUE=DATE-TIME:20111012T165000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-52@cern.ch DESCRIPTION:Speakers: KIEFT\, Gerard (Nikhef)\nThe optical modules of the future KM3NeT neutrino telescope will contain many photomultiplier tubes w ith a diameter of about three inch.\nIn order to characterize these photom ultiplier tubes\, a 16 channel Time-Over-Threshold TDC with a GigaBit Ethe rnet communication channel has been built in an Altera StratixIV evaluatio n board. The TDC data are packed in UDP packages and sent to the host PC. Control is implemented using I2C command packages send to the TDC by the h ost PC. After execution of I2C commands a result package is send back to t he host. We will present the TDC setup and first results.\n\nhttp://indico .cern.ch/contributionDisplay.py?contribId=52&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=52&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Global Neutrino Observatory DTSTART;VALUE=DATE-TIME:20111013T150000Z DTEND;VALUE=DATE-TIME:20111013T151500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-115@cern.ch DESCRIPTION:Speakers: KATZ\, Uli (Friedrich-Alexander-Univ. Erlangen (DE)) \nhttp://indico.cern.ch/contributionDisplay.py?contribId=115&sessionId=0&c onfId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=115&sessionId=0 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:HEAPNet and its ideas DTSTART;VALUE=DATE-TIME:20111013T144500Z DTEND;VALUE=DATE-TIME:20111013T150000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-114@cern.ch DESCRIPTION:Speakers: PIATTELLI\, Paolo (INFN-LNS\, Catania)\nhttp://indic o.cern.ch/contributionDisplay.py?contribId=114&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=114&sessionId=0 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:SCOTT: A time and amplitude digitizer ASIC for PMT signal processi ng using multi time over threshold technique. DTSTART;VALUE=DATE-TIME:20111013T082000Z DTEND;VALUE=DATE-TIME:20111013T084000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-88@cern.ch DESCRIPTION:Speakers: FERRY\, Sophie Catherine (CEA - Centre d'Etudes de S aclay (FR))\, FERRY\, Sophie ()\nThe observation of high energy neutrinos produced in astrophysical phenomena would open a new window on the Univers e. The very low neutrino cross section requires instrumented volumes at th e cubic-kilometre scale. The European KM3NeT consortium is now in a prepar atory phase towards the construction of such a large neutrino telescope in the Mediterranean Sea. Physics studies have shown that the Cherenkov ligh t produced by the neutrino induced muon must be measured with a timing pre cision of less than 2ns RMS\, and a charge estimate in a dynamic range of 1 to 100 photoelectrons. To comply with the high timing demand\, a dedicat ed ASIC\, named SCOTT\, has been developed in an AMS BiCmos 0.35 μm proce ss technology. It uses up to 16 adjustable thresholds to digitise the sign als from large photomultipliers using the time-over-threshold technique. E ach threshold channel is divided into three sub-circuits: fast comparators which thresholds are set by an internal 10-bit resistor string\, a circul ar sampling memory and a “first in first out” (FIFO) digital memory. T he sampling frequency is equivalent to a conventional ADC with an 800 MHz sampling clock. A detailed study was performed to process and analyse the data output of the ASIC. In particular\, the choice of the number and leve l of the thresholds was optimised for pulses generated by a 10" photomulti plier tube. The methodology used for characterisation and the performance obtained in a broad charge dynamic range will be presented.\n\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=88&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=88&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Anisotropy of TeV cosmic rays in IceCube and IceTop DTSTART;VALUE=DATE-TIME:20111012T120000Z DTEND;VALUE=DATE-TIME:20111012T122000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-89@cern.ch DESCRIPTION:Speakers: SANTANDER\, Marcos (UW-Madison)\nThe main background to the search for astrophysical neutrino sources with large volume telesc opes is due to the muon component of extensive air showers produced in the interaction of high-energy cosmic rays with the Earth’s atmosphere. Thi s background\, however a nuisance for neutrino-event searches\, can be use d to explore certain aspects of cosmic ray physics. The high rate of muon events in large neutrino detectors provides a high-statistics data sample that can be used to look for an anisotropy in the arrival directions of th e parent cosmic ray particles at the per-mille level.\nI will report on th e observation of anisotropy in the cosmic ray data collected with the IceC ube neutrino telescope in the 20-400 TeV energy range at multiple angular scales. New data from the IceTop air shower array\, located on the ice sur face above IceCube\, shows an anisotropy that is consistent with the high- energy IceCube results. The sensitivity of IceTop to all the components of the extensive air shower will allow us to explore in more detail the char acteristics of the primary cosmic rays associated with the observed anisot ropy.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=89&session Id=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=89&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Latest progress in PMT development DTSTART;VALUE=DATE-TIME:20111013T084000Z DTEND;VALUE=DATE-TIME:20111013T090000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-111@cern.ch DESCRIPTION:Speakers: HOTTA\, Yuji (Hamamatsu Photonics K.K.)\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=111&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=111&sessionId=5 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Astrophysical Multi-messenger Observatory Network (AMON) DTSTART;VALUE=DATE-TIME:20111013T142000Z DTEND;VALUE=DATE-TIME:20111013T144500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-113@cern.ch DESCRIPTION:Speakers: Dr. DEYOUNG\, Tyce (UNIVERSITY OF MARYLAND)\nhttp:// indico.cern.ch/contributionDisplay.py?contribId=113&sessionId=0&confId=143 656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=113&sessionId=0 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Introduction DTSTART;VALUE=DATE-TIME:20111013T141000Z DTEND;VALUE=DATE-TIME:20111013T142000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-112@cern.ch DESCRIPTION:Speakers: KATZ\, Uli (Friedrich-Alexander-Univ. Erlangen (DE)) \nhttp://indico.cern.ch/contributionDisplay.py?contribId=112&sessionId=0&c onfId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=112&sessionId=0 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Reconfigurable hardware applications on NetFPGA for network monito ring in large area sensor networks DTSTART;VALUE=DATE-TIME:20111013T080000Z DTEND;VALUE=DATE-TIME:20111013T082000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-82@cern.ch DESCRIPTION:Speakers: Mr. KOUTSOUMPOS\, Vasileios (Nestor Institute for As troparticle Physics)\nA valuable functionality in many distributed\, very large volume sensor network applications is the requirement to characteriz e and analyze the data traffic at wire speed. We discuss the benefits of a reconfigurable hardware router for real-time data processing and monitori ng from sensors before the transmission to the network\, based on the NetF PGA platform. We report on our study of a hardware implementation to monit or web-based network applications and compare our results with a software based network analyzer. Finally\, we highlight the possible cases of recon figurable hardware routers\, to augment the real-time data routing\, proce ssing and monitoring tasks for large distributed sensors network such as o f a neutrino telescope.\n\nhttp://indico.cern.ch/contributionDisplay.py?co ntribId=82&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=82&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmogenic neutrinos in KM3NeT DTSTART;VALUE=DATE-TIME:20111012T134000Z DTEND;VALUE=DATE-TIME:20111012T140000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-83@cern.ch DESCRIPTION:Speakers: SHANIDZE\, Rezo (Unuversity of Erlangen)\nCosmogenic neutrinos are produced during the propagation of ultra high energy cosmic rays (UHECR) through the cosmological microwave background radiation. Ext ragalactic origin of UHECR guarantees generation of the high energy cosmo genic neutrinos\, however the flux depends on the currently unknown prope rties of UHECR\, for example the chemical composition and distribution of the sources. Estimations of cosmogenic neutrino flux\, which are constr ained by UHECR observations\, includes a range of models in which a detect able signal could be produced in a very large volume high energy neutrino telescope. In particular the favorable scenarios are based on the models with a pure proton composition of UHECR.\nThe possible event rates of cos mogenic neutrinos in KM3NeT telescope and a current status of simulations of ultra high energy neutrino events are discussed in this talk.\n\nhttp: //indico.cern.ch/contributionDisplay.py?contribId=83&sessionId=1&confId=14 3656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=83&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A DAQ processing system for the KM3NeT shore station DTSTART;VALUE=DATE-TIME:20111012T155000Z DTEND;VALUE=DATE-TIME:20111012T160500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-80@cern.ch DESCRIPTION:Speakers: Dr. PAPAIKONOMOU\, Antonis (University of Athens for the KM3NeT consortium)\nThe framework for the KM3NeT shore system is base d on the Internet Communications Engine\, ICE. The task of the system incl udes control\, data acquisition and processing\, pre-selection of events f or storage and further processing and on-line monitoring of the KM3NeT neu trino telescope. We describe the overall shore DAQ system and discuss in p articular the processing\, storing and monitoring tasks. We present our ex perience with implementations for the DAQ systems which have been build to support the foreseen demonstrator of the KM3NeT shore station.\n\nhttp:// indico.cern.ch/contributionDisplay.py?contribId=80&sessionId=8&confId=1436 56 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=80&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Time integrated search for point sources of cosmic neutrinos with the ANTARES telescope DTSTART;VALUE=DATE-TIME:20111012T143000Z DTEND;VALUE=DATE-TIME:20111012T145000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-81@cern.ch DESCRIPTION:Speakers: Mr. BOGAZZI\, Claudio (NIKHEF)\nResults of a time-in tegrated search for astrophysical high energy neutrinos are presented usin g data collected from January 2007 to December 2010 with the ANTARES neutr ino telescope. ANTARES is currently the largest neutrino detector on the N orthern Hemisphere consisting of a tri-dimensional array of 885 photomulti pliers arranged on 12 vertical lines\, placed at a depth of 2475 meters in the Mediterranean Sea near Toulon\, France.\n\nAn unbinned likelihood rat io method is used to search for signal events. The final sample consists o f 3058 events. From the simulations 84\\% of them are estimated to be neut rinos\, while the rest are mis-reconstructed atmospheric muons. A full sky survey as well as a search on a pre-defined list of candidate objects wer e performed. No evidence for a signal is found so neutrino upper limits ar e obtained. The neutrino flux sensitivity is $2.6\\times 10^{-8}$ (E/GeV)$ ^{-2}$ GeV$^{-1}$ s$^{-1}$ cm$^{-2}$ for the part of the sky that is alway s visible (declination $\\leq $-48 degrees) which corresponds to almost a factor 3 better than the previous search.\n\nhttp://indico.cern.ch/contrib utionDisplay.py?contribId=81&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=81&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Evaluation of triggering schemes for KM3NeT DTSTART;VALUE=DATE-TIME:20111012T151000Z DTEND;VALUE=DATE-TIME:20111012T153000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-86@cern.ch DESCRIPTION:Speakers: Mr. SEITZ\, Thomas (ECAP - University of Erlangen (f or the KM3NeT consortium))\nThe future neutrino telescope KM3NeT\, to be b uilt in the Mediterranean Sea\, will be the largest Cherenkov detector and will include several hundred thousands photomultiplier tubes (PMT). In th e deep sea the dominant source of PMT signals are decays of K40 and marine fauna bioluminescence. Selection of neutrino and muon events from this co ntinuous optical background signals requires the implementation of fast an d efficient data filtering algorithms. Various schemes for the filtering o f background data and the selection of neutrino and muon events were evalu ated for the KM3NeT telescope using Monte Carlo simulations. The results o btained in this study will be presented in the talk.\n\nhttp://indico.cern .ch/contributionDisplay.py?contribId=86&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=86&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Search for neutrino emission in gamma-ray flaring blazars with the ANTARES telescope DTSTART;VALUE=DATE-TIME:20111012T124000Z DTEND;VALUE=DATE-TIME:20111012T130000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-87@cern.ch DESCRIPTION:Speakers: SÁNCHEZ LOSA\, Agustín (IFIC (Spain))\nThe ANTARES telescope observes a full hemisphere of the sky all the time with a duty cycle close to 100%. This makes it well suited for an extensive observatio n of the neutrinos that can be produced in astrophysical transient sources .\nIn the surrounding medium of the blazars\, i.e. active galactic nuclei with their jets pointing almost directly through the observer\, neutrinos may be produced together with gamma-rays by hadronic interactions\, so it is expected a strong correlation between neutrinos and gamma-rays emission s. This information can be provided by the gamma-ray light curves measured by the LAT instrument on-board the Fermi satellite\, which reveals the ti me variability information of the studied sources. If the expected neutrin o flux observation is reduced to a narrow window around the assumed neutri no production period\, the background and point-source sensitivity can be drastically reduced.\nThe ANTARES data collected in 2008 has been analysed looking for the neutrinos detected in the high state period of nine brigh t and variable Fermi sources and assuming the gamma-ray light curves as th e neutrino emision time distributions. First results show a sensitivity im proved by a factor 2-3 with respect to a standard time-integrated point so urce search. The analysis has to be done with an unbinned method based on the minimization of a likelihood ratio\, applied to a subsample data of ~6 0 days of live time\, with typical widths for the flare ranging between 1 and 20 days.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=87& sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=87&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Muon Energy Reconstruction in the ANTARES Detector DTSTART;VALUE=DATE-TIME:20111012T120000Z DTEND;VALUE=DATE-TIME:20111012T122000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-84@cern.ch DESCRIPTION:Speakers: SCHNABEL\, Jutta (Universität Erlangen-Nürnberg/EC AP)\nThe energy reconstruction of both neutrino induced muons from neutrin o interactions in the vicinity of the detector and of muons from cosmic ra y air showers contributes indispensable information for a broad range of p hysics analyses\, e.g. by increasing the sensitivity in neutrino point sou rce searches or by offering access to observables such as the atmospheric neutrino spectrum. Currently four energy reconstruction methods are implem ented in the ANTARES data analysis framework\, ranging from estimates base d on photon counting and the total charge deposited in the detector to pdf -based methods and artificial neural networks. These four methods\, their performance and systematic studies of the energy resolution capabilities o f the ANTARES detector are presented.\n\nhttp://indico.cern.ch/contributio nDisplay.py?contribId=84&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=84&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Acoustic Calibration for the KM3NeT Pre-Production Module DTSTART;VALUE=DATE-TIME:20111012T130500Z DTEND;VALUE=DATE-TIME:20111012T132500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-85@cern.ch DESCRIPTION:Speakers: ENZENHÖFER\, Alexander (ANTARES)\nThe design of the KM3NeT neutrino telescope is based on flexible structures - the detection units. The highly dynamic environment in the deep sea necessitates a cont inuous monitoring of their exact position.\nA common way to perform this i s the use of acoustic emitters and receivers based on the piezoelectric ef fect. The receivers are attached to detection units whereas the emitters a re located at fixed positions on the sea floor. Either commercial or custo m-built devices are able to withstand the high ambient pressure in the dee p sea while still sensitive to small pressure variations\, e.g. caused by acoustic signals. With this system it is possible to determine the positio n of the detection unit with respect to the emitter on a centimetre scale\ , corresponding to a nanosecond precision for an optical device.\nThe KM3N eT Pre-Production Module (PPM) is a test system to verify the correct oper ation and interoperability of the major involved hardware and software com ponents. The proposed solution presented here is the use of a small piezoe lectric element equipped with preamplifiers inside the optical module in t he same housing as the optical sensors. This custom-built solution also ho lds the possibility to extend the application area from only positioning t o additional tasks like acoustic particle detection or monitoring of the b arely known deep-sea acoustic environment.\n\nhttp://indico.cern.ch/contri butionDisplay.py?contribId=85&sessionId=3&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=85&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:KM3NeT - where are we and where do we go DTSTART;VALUE=DATE-TIME:20111014T080000Z DTEND;VALUE=DATE-TIME:20111014T090000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-7@cern.ch DESCRIPTION:Speakers: KOOIJMAN\, Paul Martin (NIKHEF)\nThe talk will show the present technical status of the KM3NeT telescope.\nThe optimisation st udies for detection of Galactic super nova remnant sources will be presen ted and the present sensitivity to such sources will be reviewed. Implicat ions of the design on other science subjects will be shown. Possible scena rios for the realisation of the telescope in the near future will be given .\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=7&sessionId=0& confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=7&sessionId=0&c onfId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Parallel Session 2 - Mechanics\, Deployment and Vessels DTSTART;VALUE=DATE-TIME:20111013T080000Z DTEND;VALUE=DATE-TIME:20111013T080500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-108@cern.ch DESCRIPTION:Speakers: Prof. ANASSONTZIS\, Efstratios (University of Athens (GR))\, CIRCELLA\, Marco (INFN Bari\, Italy)\nhttp://indico.cern.ch/contr ibutionDisplay.py?contribId=108&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=108&sessionId=2 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Nautilus Marine Service GmbH - Industrial Presentation DTSTART;VALUE=DATE-TIME:20111013T100500Z DTEND;VALUE=DATE-TIME:20111013T102000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-109@cern.ch DESCRIPTION:Speakers: Dr. EGLOFF\, Frank (Nautilus Marine Services GmbH)\n http://indico.cern.ch/contributionDisplay.py?contribId=109&sessionId=2&con fId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=109&sessionId=2 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Methods for muon energy loss reconstruction in IceCube DTSTART;VALUE=DATE-TIME:20111012T122000Z DTEND;VALUE=DATE-TIME:20111012T124000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-102@cern.ch DESCRIPTION:Speakers: BOERSMA\, David (RWTH Aachen University)\nThe energy of muon neutrinos and muons detected by IceCube is not directly measured. For low energy contained events the length of the track inside can be use d to derive an energy estimate. For higher energy through-going events the main energy-related observable is the energy *loss* of muons. The stochas tic nature of this energy loss makes the reconstruction non-trivial. Sever al approaches have been developed to reconstruct the muon energy loss in I ceCube events and to derive the muon energy from that. These approaches v ary both in the level of detail of the result and in the techniques they u se to take the ice properties into account. I will present an overview of these approaches and the preliminary estimates of their performance.\n\nht tp://indico.cern.ch/contributionDisplay.py?contribId=102&sessionId=1&confI d=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=102&sessionId=1 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Point Source Searches by IceCube: Recent Results and Progress DTSTART;VALUE=DATE-TIME:20111012T145000Z DTEND;VALUE=DATE-TIME:20111012T151000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-103@cern.ch DESCRIPTION:Speakers: FINLEY\, Chad ()\, FINLEY\, Chad ()\, FINLEY\, Chad ()\nA wide range of analyses are pursued by IceCube in the search for astr ophysical sources of neutrinos. These include time-integrated searches fo r steady sources\, time-dependent searches correlated with AGN and other f lares\, and searches dedicated to GRBs as well as generic all-sky burst se arches. In addition\, an online system is now in place that sends neutrin o-triggered alerts to optical\, x-ray\, and gamma-ray telescopes for follo w-up observations. In this talk I will present recent results of point so urce searches by IceCube\, and describe progress toward maximizing the pot ential of the completed detector to discover astrophysical neutrino source s.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=103&sessionId =1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=103&sessionId=1 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Photon tracking with GPUs in IceCube DTSTART;VALUE=DATE-TIME:20111012T161000Z DTEND;VALUE=DATE-TIME:20111012T162500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-100@cern.ch DESCRIPTION:Speakers: CHIRKIN\, Dmitry (UW\, Madison\, U.S.A.)\nGPUs (grap hics processing units) have become increasingly popular in the recent year s for scientific calculations involving large numbers of similar steps. Ph oton propagation is a necessary part of simulating detector response to pa ssing charged particles in IceCube that is an ideal application for use wi th GPUs. We discuss the principle ideas and practical issues of running su ch an application within the simulation chain used within our collaboratio n.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=100&sessionId =8&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=100&sessionId=8 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Maintenance of the deep-sea ANTARES neutrino telescope DTSTART;VALUE=DATE-TIME:20111013T080500Z DTEND;VALUE=DATE-TIME:20111013T082000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-106@cern.ch DESCRIPTION:Speakers: CIRCELLA\, Marco (INFN Bari\, Italy)\nANTARES is the first neutrino telescope ever built in deep sea. The apparatus is equippe d with 885 Optical Modules arranged on 12 detection lines. The constructio n of the apparatus was completed in 2008. The Collaboration then launched a two-year maintenance campaign\, during which three lines were recovered and reinstalled\, after curing some initial functionality problems. This a ctivity has been quite successful so that the apparatus is back in the ful l 12 detection line configuration since November 2010. Furthermore\, valua ble experience toward the construction of a km3-scale apparatus has been g ained during the process. The main points of these activities will be illu strated in this talk.\n\nhttp://indico.cern.ch/contributionDisplay.py?cont ribId=106&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=106&sessionId=2 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Mechanical design of NEMO Phase 2 DTSTART;VALUE=DATE-TIME:20111013T082500Z DTEND;VALUE=DATE-TIME:20111013T084000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-107@cern.ch DESCRIPTION:Speakers: CACOPARDO\, Giorgio (INFN- LNS)\nThe NEMO Collaborat ion\, which is part of the KM3NeT consortium\, is pursuing a wide prototyp ing campaign (NEMO Phase 2)\noff the coast of Sicily. A summary of the mec hanical developments performed in this project will be presented.\n\nhttp: //indico.cern.ch/contributionDisplay.py?contribId=107&sessionId=2&confId=1 43656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=107&sessionId=2 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Common Simulation Tools for Large Volume Neutrino Detectors DTSTART;VALUE=DATE-TIME:20111013T080000Z DTEND;VALUE=DATE-TIME:20111013T083000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-104@cern.ch DESCRIPTION:Speakers: MARGIOTTA\, Annarita (Universita e INFN (IT))\nA sho rt overview of the MC simulation tools used in the ANTARES and IceCube exp eriments is given. The differences in the general approaches used by the 2 groups due to the characteristic features of the medium where the detecto rs collect data are stressed and discussed. Limitations of the present too ls are reviewed and on-going developments of new software and techniques are presented.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=1 04&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=104&sessionId=1 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Mechanical design of the Pre-Production Detector Unit Model of KM3 NeT DTSTART;VALUE=DATE-TIME:20111013T094500Z DTEND;VALUE=DATE-TIME:20111013T100000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-105@cern.ch DESCRIPTION:Speakers: MUSUMECI\, Mario (INFN)\nThe KM3NeT Consortium\, aim ing to design and prepare the deployment of a deep sea detector for high e nergy neutrino astronomy\, is developing a Pre-Production Model of the Det ection Unit (PPM-DU) of the future telescope.\nA description of the mechan ical structure of the PPM-DU\, of the R&D activity that have brought to it and of the ongoing qualification process will be presented.\n\nhttp://ind ico.cern.ch/contributionDisplay.py?contribId=105&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=105&sessionId=2 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:White Rabbit: Sub-Nanosecond Timing over Ethernet DTSTART;VALUE=DATE-TIME:20111013T100000Z DTEND;VALUE=DATE-TIME:20111013T102000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-39@cern.ch DESCRIPTION:Speakers: PEEK\, Henk (NIKHEF (NL))\nOn behalf of the White Ra bbit consortium\nThe White Rabbit (WR) project is a multi-laboratory\, mul ti-company effort to bring the best of the data transfer and the timing wo rld together in a completely open design. White Rabbit is a fully determin istic Ethernet-based network for general purpose data transfer and synchro nization. The aim is to be able to synchronize a large number of nodes wit h sub-nanosecond accuracy and picosecond jitter over long lengths of fiber . The key technologies used are physical layer syntonization (clock recove ry) and the Precision Time Protocol (IEEE 1588). It generates sub-nanoseco nd synchronous precision timing in all nodes by continuous tracking and co mpensating the fiber transmission delays.\nThis presentation/paper gives a n overview of WR and describes the design goals and specification used for the project. It describes the WR switch and the (user) node which are the central components of the WR system. Finally\, it presents real timing me asurements of prototypes of WR hardware.\n\nhttp://indico.cern.ch/contribu tionDisplay.py?contribId=39&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=39&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Data readout system utilizing photonic integrated circuit DTSTART;VALUE=DATE-TIME:20111013T094000Z DTEND;VALUE=DATE-TIME:20111013T100000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-38@cern.ch DESCRIPTION:Speakers: Mr. STOPINSKI\, Stanislaw (1. Technische Universitei t Eindhoven 2. Institute of Microelectronics and Optoelectronics of Warsaw University of Technology)\nWe describe a novel optical solution for data readout systems\, developed within the framework of the FP7 NMP project Eu roPIC (europic.jeppix.eu). In this project photonic ICs in the Indium-Phos phide-based material system are designed and fabricated. This enables the monolithic integration of active (amplifiers\, photodetectors) with modula tors and passive components (waveguides\, splitters\, filters). With these components\, circuits containing laser light sources \, receivers\, switc hes and routers can be fabricated. In comparison to bulk fiber-optic or el ectrical equivalents\, photonic integrated circuits offer advantageous per formance in terms of size and weight\, energy consumption\, operational sp eed and bit-rate.\nAlthough the specifications of the system presented her e have been taken from the KM3NeT project\, the proposed solution is suffi ciently general to make it suitable for use in other experiments. The core of the system is a photonic integrated circuit acting as a front-end read out unit. It is an optical serializer in which the serialization of an inp ut signal is provided by means of on-chip optical delay lines. The circuit employs electro-optic phase shifters to build amplitude modulators\, powe r splitters for signal distribution\, semiconductor optical amplifiers for signal amplification as well as on-chip reflectors. We present the concep t\, design and first characterization results of the fabricated devices.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=38&sessionId=5&co nfId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=38&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Welcome and Information by the Workshop Organisers DTSTART;VALUE=DATE-TIME:20111012T080000Z DTEND;VALUE=DATE-TIME:20111012T081500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-32@cern.ch DESCRIPTION:Speakers: KATZ\, Uli (Physikalisches Institut)\nhttp://indico. cern.ch/contributionDisplay.py?contribId=32&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=32&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Acceleration processes\, galactic sources\, the gamma connection DTSTART;VALUE=DATE-TIME:20111013T125000Z DTEND;VALUE=DATE-TIME:20111013T134000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-30@cern.ch DESCRIPTION:Speakers: DRURY\, Luke ()\nhttp://indico.cern.ch/contributionD isplay.py?contribId=30&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=30&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Indirect Search for Dark Matter with the ANTARES Neutrino Telescop e DTSTART;VALUE=DATE-TIME:20111012T132000Z DTEND;VALUE=DATE-TIME:20111012T134000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-37@cern.ch DESCRIPTION:Speakers: ZORNOZA GOMEZ\, Juan De Dios ()\nThe ANTARES Collabo ration is now operating the largest water Cherenkov neutrino telescope in the Nothern hemisphere. The apparatus\, completed in 2008\, comprises 12 d etection lines and a multidisciplinary instrumentation line installed at a depth of about 2500 m in the Mediterranean Sea offshore from France.\n\nT he goals of ANTARES are among others the search for astrophysical neutrino point sources and for neutrinos produced in self-annihilation of dark mat ter particles. Likely sources of the latter type of neutrino emission woul d be the Sun and the Galactic Centre\, where dark matter particles from th e galactic halo are expected to accumulate.\n\nPrior to its completion\, A NTARES has been taking data for more than a year in an intermediate setup with a five and a ten line detector configuration. Results on the search for dark matter annihilation in the Sun with the data recorded in 2007 and 2008 are presented\, as well as sensitivity studies on dark matter searc hes with the full ANTARES detector.\n\nhttp://indico.cern.ch/contributionD isplay.py?contribId=37&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=37&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Ageing Characterization on Large Area Photomultipliers DTSTART;VALUE=DATE-TIME:20111012T151000Z DTEND;VALUE=DATE-TIME:20111012T153000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-36@cern.ch DESCRIPTION:Speakers: Dr. LEONORA\, Emanuele (INFN Catania (Italy))\nAn ac curate study and measurement on the ageing effects on two large area photo multipliers has been performed for over three years. The photomultipliers were 10”\, 10 stages Hamamatsu R7081one with standard bialkali and the other one with super-bialkali photocathode. Gain\, dark count rate\, charg e and timing properties have been measured\, as well as the fraction of th e spurious pulses.\nDuring the ageing cycles\, the anode current of the tw o photomultipliers has been monitored and recorded in order to measure the total output anode charge and determining the ageing grade. The ageing co nditions have been set by the use of a 400nm led regulated to about 3 phot o-electrons at 1 MHz. The ageing process was stopped when the total charge arrived up toabout 2200-2550 C for both the PMTs. Measurements of the par ameters of the two PMTs have been performed using a 410 nm pulsed LASER in single photoelectron condition . Considering the main results\, only the gain showed a variation while all the other parameters remain quite stable . A first phase of up-drift shows an increase of the gain of about 10% and is followed by a final phase of down drift which shows a faster diminutio n of the gain of about 30%. The mechanism of the gain drift has been mode lled and compared with the results.\n\nhttp://indico.cern.ch/contributionD isplay.py?contribId=36&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=36&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Assembly and Design of the Optical Modules for the NEMO Phase-2 DTSTART;VALUE=DATE-TIME:20111012T134000Z DTEND;VALUE=DATE-TIME:20111012T140000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-35@cern.ch DESCRIPTION:Speakers: Dr. LEONORA\, Emanuele (INFN\, section of Catania)\n The NEMO collaboration has undertaken a Phase-2 project\, which aims at th e realization and installation of a new infrastructure at the deep-sea sit e of Capo Passero at 3500 m depth. To this aim\, a fully equipped 8-storey tower hosting two Optical Modules (OMs) at each end (four OMs per storey) is under construction. Following a well established procedure\, the assem bly of the 32 OMs is under completion. The designed OM consists of a larg e area photomultiplier tube (PMT) enclosed in a 13 in. pressure resistant glass sphere. The PMT is a R7081 sel \, produced by Hamamatsu\, with a 10 in. photocathode and 10 dynodes. Measurements carried out from a batch of 72 PMTs have shown high gain\, low dark count rate\, good resolution for t iming and charge.\nMechanical and optical contact between PMT and the glas s surface is ensured by an optical bi-component silicone gel. Tests were d one to choose the best composition considering optical and mechanical prop erties. A mu-metal cage is used to shield the PMT against the Earth’s ma gnetic field. The influence of the Earth’s magnetic field on the PMT per formances\, and the effects of the magnetic shield were measured accuratel y. The PMT base card circuit is produced by ISEG\, based on the NEMO speci fications. Inside the OM there are also a front-end board and an optical p ulser for timing calibration.\n\nhttp://indico.cern.ch/contributionDisplay .py?contribId=35&sessionId=6&confId=143656 LOCATION:Physics Lecture Hall HF URL:http://indico.cern.ch/contributionDisplay.py?contribId=35&sessionId=6& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Terrestrial Magnetic Field Effects on Large Photomultipliers DTSTART;VALUE=DATE-TIME:20111012T145000Z DTEND;VALUE=DATE-TIME:20111012T151000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-34@cern.ch DESCRIPTION:Speakers: Dr. LEONORA\, Emanuele (INFN\, section of Catania)\n The influence of the Earth’s magnetic field on candidate large PMTs for a cubic-kilometer-scale neutrino telescope was studied within the framewor k of the KM3NeT design study. In particular\, this study was aimed at dec iding whether the use of a magnetic shield could be avoided\, thereby redu cing cost and simplifying optical sensor module assembly. Measurements wer e performed for three Hamamatsu PMTs: two 8-inch\, R5912 types\; one with standard and the other with super-bialkali photocathode\, and a 10-inch R7 081 type with a standard bialkali photocathode. The various characteristic s of the PMTs\, such as transit time\, transit time spread\, gain\, peak-t o-valley ratio and charge resolution\, were measured while varying the PMT orientations with respect to the Earth’s magnetic field\, both with and without mu-metal cage magnetic shielding. Detection efficiency and the ra tes of spurious pulses were also investigated. In the 8-inch PMTs the impa ct of the magnetic field was found to be smaller than on the 10-inch PMT. With a mu-metal cage\, the 10-inch PMT had a similar response as the 8-inc h PMTs without a cage. The increased quantum efficiency in the 8 super-bia lkali PMT almost compensates its smaller detection surface compared to the 10” PMT. No significant effects of the Earth’s magnetic field were me asured upon transit time and the rates of spurious pulses.\n\nhttp://indic o.cern.ch/contributionDisplay.py?contribId=34&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=34&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:NEMO-SMO acoustic array: a deep-sea test of a novel acoustic posit ioning system for a km3-scale underwater neutrino telescope DTSTART;VALUE=DATE-TIME:20111012T124500Z DTEND;VALUE=DATE-TIME:20111012T130500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-60@cern.ch DESCRIPTION:Speakers: VIOLA\, Salvatore (INFN)\nWithin the activities of t he NEMO project\, the installation of a demonstrator 8-floors tower (NEMO- Phase II) at a depth of 3500m is foreseen in the next months. On board th e NEMO tower\, an array of 18 acoustic sensors will be installed permittin g acoustic positioning of the tower (detecting acoustic signals emitted by a long baseline of five acoustic beacons anchored on the sea-floor)\, aco ustic detection of biological sources and studies for acoustic neutrino de tection. \nFourteen high sensitivity and broadband (10 Hz – 70 kHz) hydr ophones\, provided by INFN\, will be managed by the SMO (Submarine Multidi sciplinary Observatory) project\; two free flooded rings hydrophones -sugg ested for possible use in the KM3NeT long-baseline- are provided by UPV in collaboration with CPPM-CNRS\; two acoustic sensors will be installed on special Opto-Acoustic Modules\, equipped with piezo-sensors developed by E CAP. The sensors' data acquisition system -fully integrated with the detec tor data transport system- is based on “all data to shore” philosophy. Signals coming from hydrophones are continuously sampled underwater at 19 2kHz/24 bit and transmitted to shore through an electro-optical cable for real-time analysis. A novel technology for underwater GPS time-stamp of da ta offshore has been implemented and tested. \nThe operation of the acoust ic array will permit long term test of sensor and electronics technologies that are proposed for the acoustic positioning system of KM3NeT.\n\nhttp: //indico.cern.ch/contributionDisplay.py?contribId=60&sessionId=3&confId=14 3656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=60&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Coincident searches for high energy neutrinos and gravitational wa ves with the ANTARES and LIGO/VIRGO detectors DTSTART;VALUE=DATE-TIME:20111012T124000Z DTEND;VALUE=DATE-TIME:20111012T130000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-62@cern.ch DESCRIPTION:Speakers: BOUHOU\, boutayeb (APC)\nA multimessenger approach w ith gravitational waves (GW) and high-energy neutrinos (HEN) is expected t o open new perspectives in the study of the most violent astrophysical pro cesses in the Universe. Several experiments (e.g. ANTARES\, IceCube\, LIGO and VIRGO) are currently recording data and searching for astrophysical s ources. A working group gathering physicists from those experiments has be en formed\, which the aim is to search for any connection between GW and H EN signals. The joint searches focus mainly on the gamma-ray bursts as pla usible sources of both GW and HEN. In this talk we present a joint analysi s effort\, and some recent progresses using data from ANTARES 5Line config uration\, and S5/VSR1 data from LIGO and Virgo.\n\nhttp://indico.cern.ch/ contributionDisplay.py?contribId=62&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=62&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The MEUST submarine infrastructure for neutrino astronomy DTSTART;VALUE=DATE-TIME:20111012T122500Z DTEND;VALUE=DATE-TIME:20111012T125000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-63@cern.ch DESCRIPTION:Speakers: Dr. VALLEE\, Claude (CPPM)\nLocated next to the exis ting ANTARES neutrino telescope site\, operational since 2008 offshore of Toulon at a depth of 2500m\, MEUST (Mediterranean Eurocentre for Underwate r Sciences and Technologies) will be a second generation submarine cabled infrastructure developed within the European projects KM3NeT and EMSO.\nTh is new cabled facility will share its high-capacity with neutrino astronom ers and marine environmental sciences.\nWe will present the foreseen layou t and functionalities of the deep sea permanent infrastructure of the MEUS T project and its technical features. The general topology of the sea bed network corresponds to the “ring option” presented in the KM3NeT TDR. The technological solutions take into account the evolution of available commercial components and the specificities of the MEUST site. Made of sta ndard components designed to be deployed gradually\, the foreseen submarin e infrastructure consists in a scalable ring network with 6 nodes uniforml y distributed at the periphery of a circular area of about 2km diameter. A t each node a bunch of 16 neutrinos detection units can be connected and a rranged on the bed in a similar way as ANTARES. The full network therefore accommodates up to one hundred detection units.\n\nhttp://indico.cern.ch/ contributionDisplay.py?contribId=63&sessionId=6&confId=143656 LOCATION:Physics Lecture Hall HF URL:http://indico.cern.ch/contributionDisplay.py?contribId=63&sessionId=6& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Current status of the BAIKAL-GVD project DTSTART;VALUE=DATE-TIME:20111014T093000Z DTEND;VALUE=DATE-TIME:20111014T100000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-64@cern.ch DESCRIPTION:Speakers: Dr. AYNUTDINOV\, Vladimir (INR RAS)\nSince 2006\, th e development of a km3-scale neutrino telescope - the Gigaton Volume Detec tor (GVD) in Lake Baikal - is the central goal of the Baikal collaboration . A prototype cluster of GVD was installed in Lake Baikal in April 2011. The cluster consists of 24 optical modules located on three strings. We pr esent selected results obtained in the course of developing and testing ke y elements and systems of GVD. We furthermore describe configuration and t echnical design of GVD.\n\nhttp://indico.cern.ch/contributionDisplay.py?co ntribId=64&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=64&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Quality control considerations for the KM3NeT very large volume ne utrino telescope DTSTART;VALUE=DATE-TIME:20111013T092500Z DTEND;VALUE=DATE-TIME:20111013T094000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-65@cern.ch DESCRIPTION:Speakers: SOLLIMA\, Calogero (INFN-Pisa)\nWithin the KM3NeT pr oject a quality management system was proposed that included a qualificati on process and a data base to store information on the design.\nThis paper highlights quality control procedures applicable to KM3NeT and describes the data base.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=6 5&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=65&sessionId=2& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Status of the PMT development for KM3NeT DTSTART;VALUE=DATE-TIME:20111012T153000Z DTEND;VALUE=DATE-TIME:20111012T155000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-66@cern.ch DESCRIPTION:Speakers: Mr. CLASSEN\, Lew (ECAP\, University of Erlangen)\nT hree companies are developing new types of 3 inch photomultiplier tubes (P MTs) for the KM3NeT project. The first PMT samples have been delivered fro m Hamamatsu (R6233mod type) and ET Enterprises (D783KFLA type) and tested. The results of these tests are presented. PMTs of these two types have be en ordered to build the the first KM3NeT developmental optical modules. ME LZ have produced new 82mm-diameter PMTs\, which are under internal tests i n the company. First delivery from MELZ is expected in October 2011. Hamam atsu have started the development of new versions of PMTs\, with better ti ming parameters and a larger photocathode. The delivery of the first sampl es of this new Hamamatsu type is expected in the Fall of 2011.\n\nhttp://i ndico.cern.ch/contributionDisplay.py?contribId=66&sessionId=5&confId=14365 6 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=66&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:PMT measurements in Antares DTSTART;VALUE=DATE-TIME:20111012T143000Z DTEND;VALUE=DATE-TIME:20111012T145000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-67@cern.ch DESCRIPTION:Speakers: Dr. KALEKIN\, Oleg (ECAP\, University of Erlangen)\n The comparison of the simulated to the real data in the Antares experiment is very important to understand the detector behavior. The observed diffe rences in the charge distribution of the background hits\, in the K40 coin cidence rate in two adjacent optical modules and in the hit residual time distribution have been investigated both by a more detailed description of the PMT and by a dedicated series of measurements. The understanding of these effects has reduced the discrepancies and improved the analysis quality. The effect of late pulses\, after pulses and angular acceptance have been taken into account or corrected. Measurements of these paramet ers have been carried out using Antares PMTs and optical modules while a m ore detailed simulation of the angular acceptance of the Antares optical m odule has been performed. The results of these studies are presented.\n\nh ttp://indico.cern.ch/contributionDisplay.py?contribId=67&sessionId=5&confI d=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=67&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Influence of Cosmic Ray Composition DTSTART;VALUE=DATE-TIME:20111012T122000Z DTEND;VALUE=DATE-TIME:20111012T124000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-68@cern.ch DESCRIPTION:Speakers: BERGHAUS\, Patrick (University of Delaware)\nThe com position of cosmic rays in the range relevant for large-volume neutrino de tectors constitutes a significant systematic uncertainty. An overview of a vailable data from other experiments will be given\, and the potential for independent measurements with a cubic-kilometer scale detector outlined.\ n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=68&sessionId=1&c onfId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=68&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Data Acquisition\, Triggering\, and Filtering at the Auger Enginee ring Radio Array DTSTART;VALUE=DATE-TIME:20111012T151000Z DTEND;VALUE=DATE-TIME:20111012T152500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-69@cern.ch DESCRIPTION:Speakers: Dr. KELLEY\, John (Radboud University Nijmegen)\nThe Auger Engineering Radio Array (AERA) is currently detecting cosmic rays\n of energies at and above 10^17 eV at the Pierre Auger Observatory\, by tri ggering on the radio emission produced in the associated air showers. Unl ike other air shower detection methods\, the radio-detection technique mus t cope with a significant background of man-made radio-frequency interfere nce\, but can provide information on shower development with a high duty c ycle. We discuss our techniques to handle the challenges of self-triggere d radio detection in a low-power autonomous array\, including triggering a nd filtering algorithms\, data acquisition design\, and communication syst ems.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=69&sessionI d=8&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=69&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:UHE Neutrino Searches DTSTART;VALUE=DATE-TIME:20111012T095500Z DTEND;VALUE=DATE-TIME:20111012T103000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-6@cern.ch DESCRIPTION:Speakers: CONNOLLY\, Amy (University College London)\nWe expec t an observable flux of neutrinos in the ultra-high energy (UHE) regime (a bove 10^18 eV) from the interactions of the highest energy cosmic rays wit h cosmic microwave background photons. I will review the latest constraint s set by neutrino telescopes which are closing in on this UHE neutrino flu x. The next generation of UHE neutrino experiments are aiming for detectio n volumes of order 100~km^3 in order to exploit a sample of these unique c osmic messengers. I will give an overview of what we can expect to come on line in the field in the coming years.\n\nhttp://indico.cern.ch/contributi onDisplay.py?contribId=6&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=6&sessionId=0&c onfId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Photomultiplier Design and Manufacture at ET Enterprises DTSTART;VALUE=DATE-TIME:20111012T161000Z DTEND;VALUE=DATE-TIME:20111012T163000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-98@cern.ch DESCRIPTION:Speakers: CORMACK\, Andy (ET Enterprises Ltd)\nET Enterprises Limited started in May 2007 and took over the photomultiplier tubes and ac cessories business of Electron Tubes Limited and will continue to manufact ure\, supply and develop the Electron Tubes brand product range. ET Enterp rises is located in Uxbridge\, which is about 30km west of London.\n\nA su bsidiary of Ludlum Measurements Inc.\, ET Enterprises Limited benefits fro m the additional production facilities of ADIT\, a US based producer of ph otomultipliers. Similarly\, ADIT\, which specialises in photomultipliers f or scintillation applications\, has access to ET Enterprises' development resources and experience in many different photomultiplier applications wo rldwide.\n\nWe present information on the company\, or manufacturing facil ities\, and our products\, with a focus on work on photomultipliers for HE P experiments with requirements for 3 inch\, 9 inch\, and 11 inch diameter pmts.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=98&sessio nId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=98&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Development of an acoustic transceiver for the KM3NeT positioning system DTSTART;VALUE=DATE-TIME:20111012T132500Z DTEND;VALUE=DATE-TIME:20111012T134500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-91@cern.ch DESCRIPTION:Speakers: Ms. LAROSA\, Giuseppina (IGIC-Universitat Politècni ca de València)\nIn this paper we describe the acoustic transceiver devel oped for the KM3NeT positioning system. The acoustic transceiver is compos ed of a commercial free flooded transducer\, which works mainly on the 20- 40 kHz region and withstands high pressures (up to 500 bars). A developed sound emission board\, which has been designed to be adapted to the specif ic transducer and fulfill all the requirements: low power consumption\, hi gh intensity for emission\, low intrinsic noise\, arbitrary signals for em ission and the capacity of acquiring the receiving signals with very good timing precision. Moreover\, a simplified version of the transceiver might be used for the receivers of the KM3NeT positioning system as well for th e large number of units needed. \nThe results of the different tests made to the transceiver in the laboratory are described\, as well as\, the acti vities for its integration in the Instrumentation Line of ANTARES and in t he NEMO tower for the in situ tests.\n\nhttp://indico.cern.ch/contribution Display.py?contribId=91&sessionId=3&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=91&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Calibration systems of the ANTARES neutrino telescope DTSTART;VALUE=DATE-TIME:20111012T120000Z DTEND;VALUE=DATE-TIME:20111012T122500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-90@cern.ch DESCRIPTION:Speakers: GÓMEZ GONZÁLEZ\, Juan Pablo (ANTARES)\nThe ANTARES neutrino telescope is a photo-detector array consisting of 12 flexible st rings holding 885 photomultiplier tubes which collect the Cherenkov light emitted by the charged leptons produced in the interaction of high energy neutrinos with the matter in or surrounding the detector. \nThe trajectori es of the resulting muons can be reconstructed using the time\, position a nd charge information of the hits arriving to the PMTS. An accurate calibr ation of each acquisition elements is demanded to ensure the best event re construction attainable and to make astronomy. This contribution reviews t he diff\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=90&sessi onId=3&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=90&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of Neutrino Oscillations with the ANTARES detector DTSTART;VALUE=DATE-TIME:20111012T130000Z DTEND;VALUE=DATE-TIME:20111012T132000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-93@cern.ch DESCRIPTION:Speakers: BRUNNER\, Juergen (Universite d'Aix - Marseille II ( FR))\nThe data taken with ANTARES from 2007 to 2010 with a total lifetime of 830 days have been analysed in view of a possible neutrino oscillation signal. The flux of vertical upward going muon neutrinos should be complet ely suppressed at energies of 24 GeV due to neutrino oscillations.\nA dedi cated algorithm is used\, which allows the reliable reconstruction of muon tracks with energies as low as 20 GeV. The oscillation signal is extracte d by comparing two event samples: a low energy sample of vertical upward g oing tracks seen on a single detector line and a higher energetic set of m ore isotropic events seen on several detector lines. The presentation will detail the analysis method\, the estimation of systematic effects and the result of the measurement of the oscillation parameters.\n\nhttp://indico .cern.ch/contributionDisplay.py?contribId=93&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=93&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The NEMO Trigger and Data Acquisition System DTSTART;VALUE=DATE-TIME:20111012T145000Z DTEND;VALUE=DATE-TIME:20111012T150500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-92@cern.ch DESCRIPTION:Speakers: CHIARUSI\, Tommaso (INFN - Sezione di Bologna)\nThe phase 2 of the NEMO project represents a unique occasion to test a new Tr igger and Data Acquisition System (TriDAS)\, designed to scale up to the k m3.\nBecause of the deep sea optical background\, the NEMO "all data t o shore" approach requires to handle a large continuous data-stream from off-shore to on-shore\, up to the last on-line computing element.\nThe co mputing layers of TriDAS start after the Ethernet Floor Control Module (e FCM) electronic boards on-shore\, which gate the data-stream arriving fro m the off-shore detector. It is arranged into 4 elements: hit managing in to time-coherent aggregates\, data selection according to possible concurr ent trigger algorithms\, composition of the selected events into a post-t rigger files and finally a persistent data storage.\nThe finalized design of TriDAS adapted for NEMO -Phase 2 is presented together with its on-l ine data monitoring environment and the dedicated networking architecture. \n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=92&sessionId=8& confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=92&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Embedded electronics and data acquisition of a detection node for the European KM3NeT telescope. DTSTART;VALUE=DATE-TIME:20111013T102000Z DTEND;VALUE=DATE-TIME:20111013T104000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-95@cern.ch DESCRIPTION:Speakers: LOUIS\, frederic (CEA)\nA KM3Net detection node cons ists of a multi-PMT Digital Optical Module(DOM) containing 31 photomultipl iers (PMTs) and the associated electronic for power\, readout and control. \nThe components of the DOM electronic will be reviewed\, namely a System -on-chip in charge of the data acquisition and slow control\, a power boar d converter\, various instrumentation devices and a Gigabit Ethernet link over an optical network to shore\nThe PMT front end signals are sampled wi th TDCs integrated in the SoC. An embedded processor is used for real time data processing and transmission to shore. The off shore electronics rece ives a bit stream from the optical network which carries both data and a s ynchronous clock signal used as a timing reference for the SoC. The overal l architecture of the SoC and its inner functionalities will be presented in detail.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=95&se ssionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=95&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction and identification of neutrino-induced particle sho wers in IceCube DTSTART;VALUE=DATE-TIME:20111013T091000Z DTEND;VALUE=DATE-TIME:20111013T093000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-94@cern.ch DESCRIPTION:Speakers: MIDDELL\, Eike (DESY)\nAn instrument like IceCube se arches for neutrinos by recording and interpreting the Cherenkov light of charged particles that traverse the instrumented volume. From the photon i ntensity and arrival times at different locations in the detector one has to discern the nature of the event\, separate neutrino candidates from the atmospheric muon background\, and derive relevant properties like the dep osited energy or the direction of the incident primary. This talk presents methods currently used to reconstruct events containing electromagnetic a nd hadronic particle showers. This class of events is important because pa rticle showers emerge from the interactions of neutrinos of all flavors an d allow for a better reconstruction of the neutrino energy compared to muo n tracks.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=94&ses sionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=94&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Online Control and Configuration in KM3NeT DTSTART;VALUE=DATE-TIME:20111012T153000Z DTEND;VALUE=DATE-TIME:20111012T154500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-97@cern.ch DESCRIPTION:Speakers: Dr. ANVAR\, Shebli (CEA - Centre d'Etudes de Saclay (FR))\nThe data acquisition infrastructure of the KM3NeT deep-sea neutrino telescope in the Mediterranean will be a massively distributed system. Th e control and configuration application will be distributed over some 2000 offshore embedded nodes and hundreds of onshore processes. The full run c onditions and detector state will have to be reliably set up and traced fo r a valid scientific analysis of the data. The actual implementation of th e online software system must also take into account the complexity of dev elopment processes involving multiple actors and laboratories. Following t he development principles established during the KM3NeT Design Study\, an implementation of the online control and configuration software framework has been developed for the KM3NeT pre-production model detection unit (PPM -DU) of the FP7 Preparatory Phase. It features a highly modular client-ser ver architecture based on specialized components communicating over the Ze roC Ice distributed application middleware. The full detector configuratio n is implemented using a framework developed for KM3NeT which provides for a coherent development process among multiple teams through features such as automatic database mapping or default parameter value broadcasting. Ke y features of the different frameworks\, their integration for the PPM-DU and the client-server architecture of the data acquisition system and its control and configuration architecture are presented.\n\nhttp://indico.cer n.ch/contributionDisplay.py?contribId=97&sessionId=8&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=97&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The Antares Computing Model DTSTART;VALUE=DATE-TIME:20111012T143000Z DTEND;VALUE=DATE-TIME:20111012T144500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-96@cern.ch DESCRIPTION:Speakers: Dr. KOPPER\, Claudio (NIKHEF (for the ANTARES collab oration))\nCompleted in 2008\, ANTARES is now the largest water Cherenkov neutrino telescope\nin the Northern Hemisphere. Its main goal is to detect neutrinos from galactic and extra-galactic sources. Due to the high backg round rate of atmospheric muons and the high level of bioluminescence\, se veral online and offline filtering algorithms have to be applied to the ra w data taken by the instrument. To be able to handle this data stream\, a dedicated computing infrastructure has been set up.\n\nThe talk will cover the main aspects of the current official Antares computing model.\nThis i ncludes an overview of online and offline data handling and storage. In ad dition\, the "IceTray" software framework\, which is used to link together the various data analysis modules\, will be presented and its current usa ge in Antares data processing will be highlighted. Finally\, an overview o f the final data storage format used for high-level analysis will be given .\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=96&sessionId=8 &confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=96&sessionId=8& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos with JEM-EUSO DTSTART;VALUE=DATE-TIME:20111014T100000Z DTEND;VALUE=DATE-TIME:20111014T103000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-10@cern.ch DESCRIPTION:Speakers: SANTANGELO\, Andrea ()\nIn this contribution we will present the Extreme Universe Space Observatory onboard the Japanese Exper iment Module of the ISS. After briefing summarize the scientific case of t he mission\, we will discuss the technological aspects and the expected pe rformance of the mission. We will then focus on the capability of JEM-EUSO in detecting neutrinos at Ultra High Energy and on the potential science outcome of the mission in neutrino astrophysics.\n\nhttp://indico.cern.ch/ contributionDisplay.py?contribId=10&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=10&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Funding aspects DTSTART;VALUE=DATE-TIME:20111014T133000Z DTEND;VALUE=DATE-TIME:20111014T140000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-13@cern.ch DESCRIPTION:Speakers: Dr. BERGHOEFER\, Thomas (PT-DESY)\nASPERA is the net work of European funding agencies in the field of astroparticle physics. I n my presentation I will report on the status of the implementation of the European roadmap for astroparticle physics and the network's supporting a ctivities in view of the realization of coming large projects including a large underwater neutrino telescope in the Mediterranean.\n\nhttp://indico .cern.ch/contributionDisplay.py?contribId=13&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=13&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Roadmaps for neutrino APP DTSTART;VALUE=DATE-TIME:20111014T130000Z DTEND;VALUE=DATE-TIME:20111014T133000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-12@cern.ch DESCRIPTION:Speakers: SPIERING\, Christian (DESY)\nThis talk will summariz e the recommendations of the ASPERA roadmap\, with a focus to high energy neutrinos. It will also relate the ASPERA strategy on neutrino projects to strategy discussions in other parts of the world.\n\nhttp://indico.cern.c h/contributionDisplay.py?contribId=12&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=12&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Welcome by the Vice-President of the University of Erlangen DTSTART;VALUE=DATE-TIME:20111012T081500Z DTEND;VALUE=DATE-TIME:20111012T083000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-14@cern.ch DESCRIPTION:Speakers: Prof. HORNEGGER\, Joachim (Friedrich-Alexander-Unive rsität Erlangen-Nürnberg)\nhttp://indico.cern.ch/contributionDisplay.py? contribId=14&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=14&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Panel Discussion DTSTART;VALUE=DATE-TIME:20111013T151500Z DTEND;VALUE=DATE-TIME:20111013T163000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-116@cern.ch DESCRIPTION:Speakers: \nhttp://indico.cern.ch/contributionDisplay.py?contr ibId=116&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=116&sessionId=0 &confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A vertical electro-optical data cable for KM3NeT DTSTART;VALUE=DATE-TIME:20111012T131500Z DTEND;VALUE=DATE-TIME:20111012T134000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-48@cern.ch DESCRIPTION:Speakers: MUL\, Gertjan (Nikhef (for the KM3NeT consortium))\n KM3NeT is a research facility which will be built at the bottom of the Med iterranean Sea. The facility will host a neutrino telescope with several h undreds of detection units - vertical mechanical structures to which the o ptical sensors modules of the telescope are attached. A data cable will ru n the full length of the structure\, which is almost one kilometre. In ord er to allow a novel compact deployment of the detection unit\, the cable m ust be flexible and at the same time protect the two copper conductors and eleven optical fibres inside. In order to comply to these requirements a pressure balanced oil-filled cable has been designed\, for which a prototy pe is being built for in-situ tests at the anticipated telescope depths of 3 to 5 km. At the level of each optical sensor module a short horizontal cable breaks out which is connected to the readout components inside the g lass sphere of the module via a novel tapered glass transit. We will prese nt the design and assembly method of the cable\, the design of the glass t ransit and the results of laboratory tests.\n\nhttp://indico.cern.ch/contr ibutionDisplay.py?contribId=48&sessionId=6&confId=143656 LOCATION:Physics Lecture Hall HF URL:http://indico.cern.ch/contributionDisplay.py?contribId=48&sessionId=6& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A launching vehicle for optical modules of a deep-sea neutrino tel escope DTSTART;VALUE=DATE-TIME:20111013T090500Z DTEND;VALUE=DATE-TIME:20111013T092000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-49@cern.ch DESCRIPTION:Speakers: DE WOLF\, Els (Nikhef/University of Amsterdam)\nKM3N eT is a future deep-sea research facility that will be built at depths bet ween three and five kilometres in the Mediterranean Sea. The facility will host a neutrino telescope consisting of several hundreds of detection uni ts - vertical mechanical structures that suspend the optical sensor module s of the telescope. During the design phase of the KM3NeT telescope\, two mechanical designs for the detection unit have been worked out\, one of wh ich is a mooring consisting of two parallel ropes with 20 optical sensor m odules attached at regular intervals\; a data cable runs along the full le ngth of the structure. For this design\, which usually is referred to as a string\, a novel deployment method using a recyclable launching vehicle h as been successfully tested during two cruises in the Ionian Sea. We will present the design and the results of the deployment tests.\n\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=49&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=49&sessionId=2& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A large surface Photomultiplier based on SiPMs DTSTART;VALUE=DATE-TIME:20111012T171000Z DTEND;VALUE=DATE-TIME:20111012T173000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-46@cern.ch DESCRIPTION:Speakers: MOLLO\, Carlos Maximiliano (INFN)\nPhotosensitive de vices represent a key solution for several current and future categories o f experiments in which light detection can be considered the main observat ion channel for physical phenomena. \nAstro-particle experiments for insta nce\, one of the most promising observation channels for passive High Ener gy Physics\, typically study energetic phenomena in which charged particle s originating from the interactions or decays of primary particles radiate Cherenkov or fluorescence light\, which is then detected by photosensitiv e devices.\nIn these fields of applications\, the relatively new Silicon P hotomultipliers (SiPM) based on the limited Geiger-mode avalanche (general ly G-APD\, Geiger Avalanche Photons Detectors)\, are starting to be extens ively studied in view of their future utilization. \nActually\, however\, their use is highly limited by their small sensitive surfaces. In order to overcome to the limits of the small dimensions of the sensitive hart of S iPM devices\, different solutions to increase their field of view are repo rted. In particular it is discussed the use of Optical Concentrators with the correct refraction index\, characteristic and geometry for the improve ment of the aperture angle of view of a SiPM device and the development of a FPGA based digital circuit that allows the combination of many Optical Concentrator +MPPC systems in order to reduce dark counts and to obtain a larger total sensitive surface.\n\nhttp://indico.cern.ch/contributionDispl ay.py?contribId=46&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=46&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A mechanical design for a detection unit for a deep-sea neutrino t elescope DTSTART;VALUE=DATE-TIME:20111013T084500Z DTEND;VALUE=DATE-TIME:20111013T090000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-47@cern.ch DESCRIPTION:Speakers: BERBEE\, Edward (Nikhef (for the KM3NeT consortium)) \nThe future KM3NeT neutrino telescope will be built on the seabed of the Mediterranean Sea at a depth between three and five kilometers. The high a mbient pressure\, but also the fact that the detector is hardly accessible \, put severe constraints on the mechanical design of the detection units of the telescope. A detection unit is a vertical structure which supports the optical sensors of the telescope.\nIt has a height of almost one kilom eter\; two data cables run along the full length of the structure. Simple and therefore reliable rope and cable handling during installation of the unit at the seabed is important. During installation the stability of the unit depends mostly on the hydrodynamic behavior in the vertical direction \, while when in operation\, the horizontal behavior is of more importance . In order to reduce the estimated total transport volume of about 10000 m ^3 as\, a compact design is essential.\nWe will present a mechanical desig n that has been developed during the KM3NeT Preparatory Phase following an analysis of the designs for Antares\, NEMO and Nestor and that at the sam e time complies with the requirements for use in the KM3Net detector. The experience with this design has been used as input to the design of the KM 3Net detection unit.\n\nhttp://indico.cern.ch/contributionDisplay.py?contr ibId=47&sessionId=2&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=47&sessionId=2& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A Kalman Filter approach for track reconstruction in a neutrino te lescope DTSTART;VALUE=DATE-TIME:20111013T093000Z DTEND;VALUE=DATE-TIME:20111013T095000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-44@cern.ch DESCRIPTION:Speakers: Dr. DE ROSA\, Gianfranca (Università di Napoli Fede rico II)\nIn high energy neutrino telescopes\, the detection principle rel ies on the detection of Cherenkov light emitted from an up-going muon indu ced by νμ that have penetrated the Earth.\nAt the muon energy range of i nterest in astrophysical search (namely from about 100 GeV to about 1 PeV) \, the electromagnetic showers accompanying the muon track generate Cheren kov light emitted within a few degrees of the same cone as the light from the primary particle. Furthermore\, since photon scattering in the water\, the measurement is affected by non-Gaussian noise. As a consequence\, the reconstruction of tracks in underwater Cherenkov neutrino telescopes is s trongly complicated.\nMoreover\, environmental background originates large noise counting rate. In an undersea neutrino detector\, in fact\, the dec ay of radioactive elements in the water\, mainly the β-decay of potassium isotope 40K\, generates electrons that produce Cherenkov light leading an isotropic background of photons. These photons may compromise the hit pat tern of a neutrino induced event\, and consequently the event reconstructi on\, even when coincidence methods significatively reduce the contaminatio n.\nAs result\, track reconstruction deal with a non-linear problem with a non-Gaussian measurement noise. A method for track reconstruction in a km 3 underwater neutrino telescope\, based on Gaussian Sum Filter algorithm t o take into account non-Gaussian process noise\, is presented.\n\nhttp://i ndico.cern.ch/contributionDisplay.py?contribId=44&sessionId=1&confId=14365 6 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=44&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Search for magnetic monopoles and nuclearites with the ANTARES exp eriment DTSTART;VALUE=DATE-TIME:20111012T134000Z DTEND;VALUE=DATE-TIME:20111012T140000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-45@cern.ch DESCRIPTION:Speakers: Ms. PAVALAS\, Gabriela Emilia (Institute for Space S ciences\, Bucharest\, Romania)\nThe ANTARES neutrino telescope was install ed in the Mediterranean Sea in several stages\, and was completed in 2008. It comprises a three-dimensional array of 885 Optical Modules distributed on 12 vertical lines\, anchored at a depth of 2475 m. While designed to o bserve upgoing neutrinos\, ANTARES could also be sensitive to the bright s ignal of relativistic magnetic monopoles and slow nuclearites.\n\nMagnetic monopoles are stable particles first predicted by Dirac in 1931\, and dec ades later in various Grand Unified Theories (GUT). Relativistic magnetic monopoles would produce a large amount of Cherenkov light in the detector\ , surpassing by 8500 times the intensity of light emitted by a muon. \nA d edicated analysis and a new upper limit on the magnetic monopole flux\, ex tracted from ANTARES data taken in 2008\, is presented.\n\nNuclearites are massive particles of strange quark matter that may be present in the cosm ic radiation. Their origin could be in the early Universe or in energetic astrophysical phenomena\, like supernovae or strange stars collisions. Nuc learites are supposed to be neutral particles and to interact with the sur rounding media via elastic and quasi elastic collisions.\nThe search strat egy and the preliminary upper limit for a nuclearite flux will be presente d\, using data collected during 2007 and 2008.\n\nhttp://indico.cern.ch/co ntributionDisplay.py?contribId=45&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=45&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of optical properties of the site of the ANTARES neutrino telescope DTSTART;VALUE=DATE-TIME:20111012T122500Z DTEND;VALUE=DATE-TIME:20111012T124500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-42@cern.ch DESCRIPTION:Speakers: YEPES RAMIREZ\, Harold (IFIC-ANTARES)\nANTARES is a neutrino detector based on a three dimensional grid of photomultipliers tu bes (PMTs) arranged in several detection lines anchored to the seabed at 2 .5 km of deep into the Mediterranean Sea (40 km o\n\nhttp://indico.cern.ch /contributionDisplay.py?contribId=42&sessionId=3&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=42&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:VSiPMT for underwater neutrino telescopes DTSTART;VALUE=DATE-TIME:20111012T165000Z DTEND;VALUE=DATE-TIME:20111012T171000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-43@cern.ch DESCRIPTION:Speakers: Dr. VIVOLO\, Daniele (Università degli Studi di Nap oli "Federico II" e INFN)\nUnderwater neutrino telescopes are nowadays con sidered as one of the most important aims in the astroparticle physics fie ld. Their structure consists of a cubic-kilometer three dimensional array of photosensitive devices aimed at the detection of the Cherenkov light e mitted by charged particles produced by high energy neutrino interactions with Earth. To date\, a crucial role in this kind of experiments has been played by PhotoMultiplier Tubes (PMTs)\, however they suffer of many drawb acks such as linearity-to-gain relationship and difficulty in single photo n counting. The next generation of experiments will require further improv ements in photon detectors performances\, therefore alternatives to PMTs a re under study. In particular the most promising development in this field is represented by the rapidly emerging CMOS p-n Geiger-mode avalanche pho todiode technology (G-APD or SiPM)\, that will allow the detection of high speed single photons response with high gain and linearity. In order to o vercome to the limits of its small sensitive surface we propose an innovat ive design for a modern hybrid\, high gain\, silicon based Vacuum Silicon Photomultiplier Tube (VSiPMT) based on the combination of a SiPM with a he mispherical vacuum glass PMT standard envelope.\nIn this work we describe the full SiPM characterization realized by our group and present the resul ts of our Geant4-based simulations of backscattering of electrons over SiP M surface.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=43&se ssionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=43&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Ultra-High-Energy neutrinos at the Pierre Auger Observa tory DTSTART;VALUE=DATE-TIME:20111012T132000Z DTEND;VALUE=DATE-TIME:20111012T134000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-40@cern.ch DESCRIPTION:Speakers: GONZALEZ\, Javier (KIT)\nThe Pierre Auger Observator y is sensitive to extended air-showers induced by ultra-high-energy neutri nos of all flavors as they interact with the atmosphere and inside the ear th. These air-showers display characteristic features that allow their ide ntification. We report on recent searches for ultra-high-energy neutrinos at the Pierre Auger Observatory. We present the different identification c riteria used\, discuss the sources of background and systematic uncertaint ies\, and place the corresponding limits on the neutrino fluxes.\n\nhttp:/ /indico.cern.ch/contributionDisplay.py?contribId=40&sessionId=1&confId=143 656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=40&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Development of a compact acoustic calibrator for ultra-high energy neutrino detection DTSTART;VALUE=DATE-TIME:20111012T134500Z DTEND;VALUE=DATE-TIME:20111012T140000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-41@cern.ch DESCRIPTION:Speakers: Ms. ADRIÁN\, Silvia (Antares-UPV)\nWith the aim to optimize and test the acoustic detection of ultra-high energy neutrinos in underwater telescopes\, we have developed a compact acoustic transmitter array able to reproduce the acoustic signature of UHE neutrino based on th e parametric acoustic sources effect. We present different R&D studies to show the viability of the parametric sources technique to deal with the di fficulties of generating the acoustic signal (a very directive transient b ipolar signal with ‘pancake’ directivity). The design\, building and c haracterization of the prototype is described\, including theoretical simu lations of several waveforms propagation at km range the experimental meas ures in a pool. Following these studies\, next steps will be to test the d evice in situ\, in underwater neutrino telescopes or from a vessel in Sea Campaigns.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=41&se ssionId=3&confId=143656 LOCATION:Physics Lecture Hall HH URL:http://indico.cern.ch/contributionDisplay.py?contribId=41&sessionId=3& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Northern Hemisphere Neutrino Telescopes DTSTART;VALUE=DATE-TIME:20111012T092000Z DTEND;VALUE=DATE-TIME:20111012T095500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-5@cern.ch DESCRIPTION:Speakers: HERNANDEZ-REY\, Juan (Universidad de Valencia (ES))\ nThe main features and performances of the Antares and Baikal neutrino tel escopes are reviewed. The results obtained by these detectors in several s tudies\, such as the search for neutrino point sources and diffuse fluxes\ , the search for neutrinos in coincidence with optical\, high-energy gamma and gravitational wave signals\, as well as the indirect search for dark matter and a short summary of other analyses will be presented.\n\nhttp:// indico.cern.ch/contributionDisplay.py?contribId=5&sessionId=0&confId=14365 6 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=5&sessionId=0&c onfId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:KM3NeT deep-sea cabled network: the star-like layout DTSTART;VALUE=DATE-TIME:20111012T120000Z DTEND;VALUE=DATE-TIME:20111012T122500Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-77@cern.ch DESCRIPTION:Speakers: COCIMANO\, Rosanna (INFN-LNS)\nKM3NeT is a future de ep-sea research infrastructure hosting a neutrino telescope with a volume of more than one cubic kilometre to be constructed in the Mediterranean Se a. In the context of the Preparatory Phase of KM3NeT\, funded by the EU FP 7 framework\, the engineering design of the deep-sea telescope has been ca rried out and optimized to prepare rapid and efficient construction. This paper presents the technical solutions that have been developed for the co nstruction of the deep sea floor network. Special focus will be on the sta r-like subsea network with emphasis on the electrical power system\, the d eep-sea electro-optical cables\, the connection systems and the junction b oxes.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=77&session Id=6&confId=143656 LOCATION:Physics Lecture Hall HF URL:http://indico.cern.ch/contributionDisplay.py?contribId=77&sessionId=6& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Evaluation of the discovery potential of an underwater Mediterrane an neutrino telescope taking into account the estimated directional resolu tion and energy of the reconstructed track DTSTART;VALUE=DATE-TIME:20111013T101000Z DTEND;VALUE=DATE-TIME:20111013T103000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-76@cern.ch DESCRIPTION:Speakers: Prof. TZAMARIAS\, Spyros (Hellenic Open University)\ nWe report on the development of search methods for point like and extende d neutrino sources taking into account the resolution of an underwater Med iterranean neutrino telescope to reconstruct the direction as well as the energy of the detected muon tracks\, on a track by track basis. We present results on the potential of a very large volume neutrino telescope to dis cover neutrino sources. The developed techniques offer an improvement on t he telescope’s discovery flux sensitivity up to a factor of 2. We also r eport comparisons between different telescope configurations containing th e same number of Optical Modules.\n\nhttp://indico.cern.ch/contributionDis play.py?contribId=76&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=76&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A feasibility study for the detection of Super Nova explosions wit h an Underwater Neutrino Telescope DTSTART;VALUE=DATE-TIME:20111012T130000Z DTEND;VALUE=DATE-TIME:20111012T132000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-75@cern.ch DESCRIPTION:Speakers: Dr. LEISOS\, Anthony (Hellenic Open University Schoo l of Science & Technology)\nWe investigate the potential of a Very Large V olume Underwater Neutrino Telescope to observe Super Nova explosions withi n our Galaxy. The intense neutrino burst emitted in a SN explosion results in a large number of MeV neutrinos in the vicinity of the Neutrino Telesc ope which can be detected (mainly) via the reaction $\\bar{\\nu}_e +p \\ri ghtarrow e^{+}+n$. For the simulation study we have used the HOURS package assuming the anti electron neutrino flux of the Garching model for SN exp losions and an underwater Neutrino Telescope with 6000 direction sensitive Optical Modules each containing 31 small PMTs. Multiple Coincidences betw een the photomultiplier tubes of the same Optical Module are used to suppr ess the noise produced by $K^{40}$ decays and to establish a statistical s ignificant measurement of the neutrino flux.\n\nhttp://indico.cern.ch/cont ributionDisplay.py?contribId=75&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=75&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:A reconstruction method for neutrino induced muon tracks taking in to account the apriori knowledge of the neutrino source DTSTART;VALUE=DATE-TIME:20111013T095000Z DTEND;VALUE=DATE-TIME:20111013T101000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-74@cern.ch DESCRIPTION:Speakers: Dr. TSIRIGOTIS\, Apostolos (Physics Laboratory\, Sch ool of Science & Technology\, Hellenic Open University)\nGamma ray earthbo und & satellite experiments have observed over the last years many Galacti c and extragalactic gamma ray sources. The detection of astrophysical neut rinos emitted by the same sources would imply that these astrophysical obj ects are charged cosmic ray accelerators and help to resolve the enigma of the origin of cosmic rays. A very large volume neutrino telescope will be able to detect these potential neutrino emitters. The apriori known direc tion of the neutrino source can be used effectively to suppress the $^{40} K$ optical background through causality filters. We report on advanced fil tering and prefit techniques using the known neutrino source direction and first results are presented.\n\nhttp://indico.cern.ch/contributionDisplay .py?contribId=74&sessionId=1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=74&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction efficiency and discovery potential of a Mediterrane an neutrino telescope: A simulation study using the Hellenic Open Universi ty Simulation & Reconstruction (HOURS) package DTSTART;VALUE=DATE-TIME:20111012T155000Z DTEND;VALUE=DATE-TIME:20111012T161000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-73@cern.ch DESCRIPTION:Speakers: Dr. TSIRIGOTIS\, Apostolos (HOU)\nWe report on the e valuation of the performance of a Mediterranean very large volume neutrino telescope. We present results of our studies concerning the capability of the telescope in detecting/discovering galactic (steady point sources) an d extragalactic\, transient (Gamma Ray Bursts) high energy neutrino source s as well as measuring ultra high energy diffuse neutrino fluxes. The neut rino effective area and angular resolution are presented as a function of the neutrino energy\, and the background event rate (atmospheric neutrinos and muons) is estimated. The discovery potential of the neutrino telescop e is evaluated and the experimental time required for a significant discov ery of potential neutrino emitters (known from their gamma ray emission\, assumedly produced by hadronic interactions) is estimated. For the simulat ion we use the HOU Reconstruction & Simulation (HOURS) software package.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=73&sessionId=1&co nfId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=73&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Performance of Photo-Sensors for KM3NeT DTSTART;VALUE=DATE-TIME:20111012T155000Z DTEND;VALUE=DATE-TIME:20111012T161000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-72@cern.ch DESCRIPTION:Speakers: DOROSTI\, Qader (KVI Groningen)\nKM3NeT\, the future deep-sea neutrino telescope of multi-cubic km size\, is being designed to search for high energy neutrinos originating from galactic and extragalac tic sources. The neutrinos can be detected by collecting Cherenkov light e mitted from relativistic charged secondary particles caused by the interac tion of neutrinos with the medium surrounding the detector. To collect the Cherenkov light\, an optical module (OM) containing an array of 31 3-inch diameter photomultiplier tubes (PMTs) has been designed as a promising al ternative to an OM containing one 10-inch diameter PMT. The main advantage is to reduce the environmental background by requiring local coincidences between neighbouring photo sensors and to provide a homogeneous photon ac ceptance. Optimum performance requires high collection efficiency at low d ark noise\, homogeneous photocathode response and excellent timing propert ies. \nWe studied the response to single photo-electrons of a newly develo ped 3-inch diameter PMT from Electron Tube Enterprises Ltd.. To study the timing and homogeneity of the PMT\, we employed a 2D scanning system with a picosecond-laser (timing precision \n\nhttp://indico.cern.ch/contributi onDisplay.py?contribId=72&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=72&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino-induced showers in the ANTARES Deep-Sea Telescope DTSTART;VALUE=DATE-TIME:20111013T085000Z DTEND;VALUE=DATE-TIME:20111013T091000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-71@cern.ch DESCRIPTION:Speakers: DOROSTI\, Qader (KVI Groningen)\nThe ANTARES neutrin o telescope operating in the Mediterranean Sea aims to measure the cosmic neutrino flux and locate point sources in the multi-TeV energy range. Prim arily this is achieved by detecting up-going muon tracks caused by charged -current interactions of neutrinos having passed through the Earth. Neutri no-induced showers\, initiated by neutral-current interactions\, extend th e sensitivity of the detector to all neutrino flavors. A major challenge in reconstructing showers is their identification within an overwhelming b ackground of down-going atmospheric muons. We have developed a strategy to select up-going showers with high efficiency and purity. Atmospheric muon s are suppressed largely by estimating the shower direction from the direc tion of light emission and rejecting down-going events. In addition\, even ts are selected with a large amount of collected charge. We estimate the m ean space-time position of the shower vertex\, assuming that the shower li ght is emitted from a bright point\, and refine the estimate by an M-estim ator fit. By combining the quality cuts on observables describing the show er structure\, we are able to reconstruct showers with high purity and a s election efficiency of about 22%. The parameters of the selection strategy are tuned on Monte-Carlo simulations producing the proper amount of backg round and atmospheric neutrino-induced showers. The method has been applie d to ANTARES experimental data and the performance results will be discuss ed.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=71&sessionId =1&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=71&sessionId=1& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:The Askaryan Radio Array DTSTART;VALUE=DATE-TIME:20111014T120000Z DTEND;VALUE=DATE-TIME:20111014T123000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-70@cern.ch DESCRIPTION:Speakers: HANSON\, Kael (Université Libre de Bruxelles)\nThe ARA collaboration is developing an array of radiofrequency antennas coveri ng approx. 150 sq-km surface which will be installed in boreholes extendin g 200 m below the ice surface at the geographic South Pole. The antennas a re senstitive to the weak\, transient impulses given off by exteremely hig h energy neutrino-induced cascades. The array geometry has been chosen to ensure the detection of the flux of neutrinos guaranteed by observations of the GZK cutoff by HiRes and the Pierre Auger Observatory. The first com ponents of ARA have been installed during the austral summer of 2010-2011 and have proven that the South Pole site is an optimal environment for suc h a detector. After three years of operation\, the full array sensitivity will exceed that of any other instrument in the 0.1-10 EeV energy range by an order of magnitude. The primary goal of the ARA experiment is to estab lish the absolute cosmogenic neutrino flux through a modest number of even ts. This talk will describe the array\, its science goals\, and give the c urrent status of the project.\n\nhttp://indico.cern.ch/contributionDisplay .py?contribId=70&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=70&sessionId=0& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:FPGA shore station demonstrator for KM3NeT DTSTART;VALUE=DATE-TIME:20111013T090000Z DTEND;VALUE=DATE-TIME:20111013T092000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-79@cern.ch DESCRIPTION:Speakers: Dr. MANOLOPOULOS\, Kostas (NESTOR Institute for Astr oparticle Physics for the KM3NeT consortium)\nThe KM3NeT readout concept i s based on a point-to-point optical network connecting the ten thousand op tical modules in the deep-sea neutrino telescope with the shore station. T he numerous fibre optic channels arriving at the shore station will be con centrated on the shore electronics systems\, which will receive\, merge an d time order the data\, and send them to the DAQ system. Although the net work functionality is bi-directional\, the physical channel allocation is asymmetric\; most channels are assigned to the data reception and only a f ew channels are used for control with data transport from shore to the tel escope.\nWe will discuss the FPGA based platform systems for the shore sta tion and the appropriate firmware implementation for the data gathering an d broadcast demands of a neutrino telescope. We will present our experienc es based on FPGA evaluation platforms suitable to build a demonstrator of the KM3NeT shore station.\n\nhttp://indico.cern.ch/contributionDisplay.py? contribId=79&sessionId=5&confId=143656 LOCATION:Physics Lecture Hall HE URL:http://indico.cern.ch/contributionDisplay.py?contribId=79&sessionId=5& confId=143656 END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Detection\, Position Calibration and Marine Science with Acoustic Arrays in the Deep Sea DTSTART;VALUE=DATE-TIME:20111014T123000Z DTEND;VALUE=DATE-TIME:20111014T130000Z DTSTAMP;VALUE=DATE-TIME:20130520T060212Z UID:indico-contribution-143656-78@cern.ch DESCRIPTION:Speakers: LAHMANN\, Robert (Friedrich-Alexander-Univ. Erlangen (DE))\nArrays of acoustic receivers are an integral part of present and p otential future Cherenkov neutrino telescopes in the deep sea. They are re quired to monitor the positions of the optical detection modules whose pos itions vary with time as an effect of undersea currents. At the same time\ , the acoustic receivers can be employed for marine science purposes\, in particular for monitoring the ambient noise environment and the signals em itted by the fauna of the sea. And last not least\, they can be used for s tudies towards acoustic detection of ultra-high energy neutrinos. Measurin g acoustic pressure pulses in huge underwater acoustic arrays\, exceeding an instrumented volume of 10 km^3\, is a promising approach for the detect ion of cosmic neutrinos with energies exceeding 1 EeV. The pressure signal s are produced by the particle cascades that evolve when neutrinos interac t with nuclei in water and can be detected over large distances in the kil ometre range. In this talk\, the status of acoustic detection will be\nrev iewed and plans for the future — most notably in the context of KM3NeT — will be discussed. The connection between neutrino detection\, positio n calibration and marine science will be illustrated.\n\nhttp://indico.cer n.ch/contributionDisplay.py?contribId=78&sessionId=0&confId=143656 LOCATION:Physics Lecture Hall HG URL:http://indico.cern.ch/contributionDisplay.py?contribId=78&sessionId=0& confId=143656 END:VEVENT END:VCALENDAR