BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Recent developments at the Auger Engineering Radio Array DTSTART;VALUE=DATE-TIME:20120619T154000Z DTEND;VALUE=DATE-TIME:20120619T160500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-30@cern.ch DESCRIPTION:Speakers: MELISSAS\, Maximilien (KIT\, IEKP)\nThe first phase of the Auger Engineering Radio Array (AERA) has been deployed in the fall of 2010. Currently\, the array consists currently of 24 stations distribut ed over an area of 0.5 km$^2$. AERA has two different objectives. The fir st one is to measure cosmic-ray events and to provide the necessary data t o improve our understanding of radio emission from air showers. The second objective is to develop and test the instrumentation for the next generat ion of MHz radio-detection setups for air shower studies based on self-tri ggering methods. \n\nWith this first phase of AERA self-triggered events h ave been registered and were used for physics analysis. Moreover\, various types of hardware and different trigger strategies for the next stages in cluding cross-triggering with the surface detector are being tested with t he current setup.\nThe talk will firstly report the current status of the detector. Then\, it will focus on the available events and show comparison s between measured data and simulations and summarize the ongoing analyses . Finally we will discuss the plan for the next phase in 2012-2013.\n\nhtt p://indico.cern.ch/contributionDisplay.py?contribId=30&sessionId=7&confId= 159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=30&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Theory and simulations of air shower radio emission DTSTART;VALUE=DATE-TIME:20120620T123000Z DTEND;VALUE=DATE-TIME:20120620T131000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-54@cern.ch DESCRIPTION:Speakers: HUEGE\, Tim (KIT)\nA precise understanding of th e radio emission from extensive air showers is of fundamental import ance for the design of cosmic ray radio detectors as well as the analy sis and interpretation of their data.\n\nIn recent years\, tremendou s progress has been made in the understanding of the emission physics both in macroscopic and microscopic frameworks. A consistent p icture has emerged: the emission stems mainly from time-varying transvers e currents and a time-varying charge excess\; in addition\, Cherenkov-like compression of the emission due to the refractive index gradient in t he atmosphere can lead to high-frequency contributions in the signal.\n\nI n this overview talk\, I will discuss this the emission physics as it is understood today\, present the signatures that experiments are expec ted to see and exploit\, and conclude with a description of the models currently on the market.\n\nhttp://indico.cern.ch/contributionDisplay.py?c ontribId=54&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=54&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Searching for neutrino radio flashes from the Moon with LOFAR DTSTART;VALUE=DATE-TIME:20120619T133500Z DTEND;VALUE=DATE-TIME:20120619T135500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-28@cern.ch DESCRIPTION:Speakers: BUITINK\, Stijn (Rijksuniversiteit Groningen)\nDetec tion of ultra-high-energy neutrinos requires vast natural\ndetector volume s of ice or rock. The Moon itself is the largest\ndetector mass available. Earthbound radio telescopes can search the\nLunar surface for radio flash es\, produced by neutrinos through the\nAskaryan mechanism. A new generati on of low-frequency\, digital radio\narrays\, spearheaded by LOFAR\, will allow for searches of unprecedented\nsensitivity.\n\nThe NuMoon program ai ms to use LOFAR to search the Moon for neutrino or cosmic-ray induced radi o flashes. In this talk I will present the progress that is being made to prepare the instrument for NuMoon science runs\, and discuss the experimen tal challenges and expected sensitivity.\n\nhttp://indico.cern.ch/contribu tionDisplay.py?contribId=28&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=28&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Detection of cosmic rays using microwave radiation at the Pierre A uger Observatory DTSTART;VALUE=DATE-TIME:20120621T144000Z DTEND;VALUE=DATE-TIME:20120621T150000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-43@cern.ch DESCRIPTION:Speakers: FACAL SAN LUIS\, Pedro (University of Chicago)\nRadi ation in the microwave band from the passage of charged particles has been measured in accelerator test beams. This radiation could provide a new te chnique for ultra-high energy cosmic rays\, its main advantage being the p ossibility to instrument a large area\, with 100% duty cycle and virtually no atmospheric attenuation\, using relatively cheap equipment. Cosmic ray detection in the GHz band is being actively pursued at the Pierre Auger O bservatory with three different set-ups: MIDAS and AMBER are prototypes of an imaging parabolic dish detector\, while EASIER instruments a surface d etector tank with a radio receiver of wide angular coverage. The status of microwave R&D activities at Auger\, including the first event detected by EASIER\, will be reported.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=43&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=43&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Extensive air shower detection with CROME in the L-Band DTSTART;VALUE=DATE-TIME:20120621T135000Z DTEND;VALUE=DATE-TIME:20120621T141000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-60@cern.ch DESCRIPTION:Speakers: MATHYS\, Sebastian (Bergische Universität Wuppertal )\nExtensive air showers are detected via particle measurements on the gro und\, the energy deposition in the atmosphere or via MHz-radio waves produ ced mainly by charged particles moving in the magnetic field of the earth. In addition\, emission is predicted due to molecular bremsstrahlung. The Cosmic-Ray Observation via Microwave Emission (CROME) setup at the Karlsru he Institute of Technology (KIT) consists of several antennas in the L-ban d\, the C-band and the Ku-band. The KASCADE-Grande detector\, which trigge rs the CROME experiment\, provides calibrated measurements of air showers at the same location. In this talk the setup of a L-Band antenna\, the sig nal chain including the data acquisition and first results will be present ed. Long-term background measurements to determine the environmental backg round noise which show temporary monofrequent emitting interferences will be discussed.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=60 &sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=60&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Introduction DTSTART;VALUE=DATE-TIME:20120619T120000Z DTEND;VALUE=DATE-TIME:20120619T121500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-62@cern.ch DESCRIPTION:Speakers: LAHMANN\, Robert (Friedrich-Alexander-Univ. Erlangen (DE))\nhttp://indico.cern.ch/contributionDisplay.py?contribId=62&sessionI d=0&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=62&sessionId=0& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Welcome Address DTSTART;VALUE=DATE-TIME:20120619T121500Z DTEND;VALUE=DATE-TIME:20120619T123000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-63@cern.ch DESCRIPTION:Speakers: Prof. HORNEGGER\, J. (Vice President\, University of Erlangen-Nuremberg)\nhttp://indico.cern.ch/contributionDisplay.py?contrib Id=63&sessionId=0&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=63&sessionId=0& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Closing Address DTSTART;VALUE=DATE-TIME:20120622T104000Z DTEND;VALUE=DATE-TIME:20120622T110500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-64@cern.ch DESCRIPTION:Speakers: LAHMANN\, Robert (Friedrich-Alexander-Univ. Erlangen (DE))\nhttp://indico.cern.ch/contributionDisplay.py?contribId=64&confId=1 59364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=64&confId=15936 4 END:VEVENT BEGIN:VEVENT SUMMARY:Some possible interpretations from data of the CODALEMA experiment DTSTART;VALUE=DATE-TIME:20120620T160500Z DTEND;VALUE=DATE-TIME:20120620T163000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-53@cern.ch DESCRIPTION:Speakers: LAUTRIDOU\, Pascal (SUBATECH)\nThe purpose of the CO DALEMA experiment\, installed at the Nançay Radio Observatory (France)\, is to study the radio-detection of cosmic rays of ultra high energy. Distr ibuted over an area of 0.25 km2\, the original device has a centralized ac quisition\, and uses in coincidence an array of particle detectors and an array of active dipoles. A new analysis of energy observables is presented from this system\, taking advantage of anterior results like the geomagne tic effect or the contribution of the charge excess. Since early in 2011\, a new array of radio-detectors\, consisting of 60 stand-alone and self-tr iggered stations\, is being deployed over an area of 1.5 km2 around the in itial configuration. This new development leads to specific constraints to be discussed in term of recognition of cosmic rays and in term of analysi s of wave-front.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId =53&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=53&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Acoustic Neutrino Detection in Water DTSTART;VALUE=DATE-TIME:20120620T070000Z DTEND;VALUE=DATE-TIME:20120620T074000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-34@cern.ch DESCRIPTION:Speakers: Dr. GRAF\, Kay (University of Erlangen)\nThe acousti c neutrino detection technique is a promising approach for future large-sc ale detectors with the aim of measuring the small expected flux of ultra-h igh energy cosmogenic neutrinos. This talk will focus on the application o f the technique in water\, based on site studies performed with different acoustic test arrays. Though the technique is intriguingly simple\, challe nges arise from e.g. anisotropic sound propagation\, ambient noise or tran sient background in a natural environment. We will discuss those challenge s and the strategies to face them\, as well as developments in the simulat ion of the acoustic signal and hardware developments for sensors and calib ration sources. Furthermore\, current physics results towards the acoustic detection of ultra-high energy neutrinos in water will be presented. The acoustic detection technique will be investigated further in the next gene ration of Cherenkov neutrino telescopes that is currently prepared. We wil l discuss the technical implementation into those large optical detectors that is based on the experience gained with the acoustic test arrays.\n\nh ttp://indico.cern.ch/contributionDisplay.py?contribId=34&sessionId=8&confI d=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=34&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Development of 12 Parabolas Observation System to Detect MBR from Airshowers. DTSTART;VALUE=DATE-TIME:20120621T150000Z DTEND;VALUE=DATE-TIME:20120621T152000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-23@cern.ch DESCRIPTION:Speakers: Mr. YAMAMOTO\, Tokonatsu (Konan University)\nAn obse rvation system of MBR from extensive airshowers is being developed on a ro of of the Konan University in Japan. This system consists of 12 parabolas with 1.2 diameters. Each parabola has a 12 GHz receiver. The signals from the receivers are digitized by 65 MS/s FADC. Field of view of each parabol a is about 1.5 degrees and this system covers 6 times 4.5 square degrees. Test observation has been started since March this year and measuring nois es from the city nearby. The detail of this MBR observation system and its extension plan will be presented.\n\nhttp://indico.cern.ch/contributionDi splay.py?contribId=23&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=23&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:The Askaryan Radio Array DTSTART;VALUE=DATE-TIME:20120620T101000Z DTEND;VALUE=DATE-TIME:20120620T103500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-24@cern.ch DESCRIPTION:Speakers: MEURES\, Thomas (Université libre de Bruxelles)\nTh e Askar'yan Radio Array (ARA)\, a neutrino detector to be situated at the South Pole next to the IceCube detector\, will be sensitive to ultrahigh-e nergy cosmic neutrinos above 0.1 EeV and will have the greatest sensitivit y within the favored energy range from 0.1 EeV up to 10 EeV. Neutrinos of this energy are guaranteed by the current observations of the GZK-cutoff b y the HiRes and the Pierre Auger Observatories. The detection method is ba sed on Cherenkov emission by a neutrino induced cascade in the ice\, coher ent at radio wavelengths\, which was predicted by Askar'yan in 1962 and ve rified in beam tests at SLAC in 2006.\nThe detector is planned to consist of 37 stations with 16 antennas each\, deployed at depth of up to 200 m un der the ice surface. During the last two polar seasons (2010 -2011\, 2011 - 2012)\, a prototype station and a first detector station were successful ly deployed and are taking data. These data have been and are currently be ing analyzed concerning different measurement conditions\, which are the a mbient noise background and the properties of the South Pole ice sheet. A worldwide collaboration of people is working on the planning\, constructio n and data analysis of the detector array.\nThis presentation will give a report on the status of the ARA detector and show recent results from the recorded data.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=2 4&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=24&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Reconstructing energy and Xmax of cosmic ray air showers using the radio lateral distribution measured with LOPES DTSTART;VALUE=DATE-TIME:20120620T154500Z DTEND;VALUE=DATE-TIME:20120620T160500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-26@cern.ch DESCRIPTION:Speakers: Mrs. PALMIERI\, Nunzia (Institut fuer Kernphysik (IK P)\, Karlsruhe Institute of Technology (KIT))\nIn the previous decades\, r emarkable progress has been made in the detection of electromagnetic emiss ion from cosmic ray air showers. The LOPES experiment\, a digital radio in terferometer located at KIT (Karlsruhe Institute of Technology)\, obtained considerable results for the detection at MHz frequencies.\nAiming to bec ome competitive with the well-established investigation methods\, radio de tection has the main purpose of retrieving the complete information from a high-energy cosmic ray\, e.g. arrival direction\, energy and type of the primary particle.\nFeatures of the radio lateral distribution function (LD F) are explored in this work for a precise reconstruction of two fundament al air shower parameters: the primary energy and the shower Xmax. The met hod presented here has been developed on\n(REAS3-)simulations\, and is app lied to LOPES measurements. Despite the high human-made noise at the LOPES site\, it is possible to reconstruct both the energy and Xmax for individ ual events. While the energy resolution is promising and comparable to the one of the co-located KASCADE-Grande experiment\, the investigation shows that for a Xmax resolution better than 30 g/cm2\, a region with a lower h uman-made noise level would be needed.\n\nhttp://indico.cern.ch/contributi onDisplay.py?contribId=26&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=26&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of a phase of a radio wave reflected from rock salt an d ice irradiated by an electron beam for detection of ultra-high-energy ne utrinos DTSTART;VALUE=DATE-TIME:20120620T103500Z DTEND;VALUE=DATE-TIME:20120620T105500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-27@cern.ch DESCRIPTION:Speakers: Dr. CHIBA\, Masami (Tokyo Metropolitan University)\n We had reported a reflection effect of a radio wave from rock salt irradia ted by an X-ray or a 2MeV-electron beam. The beam irradiation had given ri se to increases in temperature and consequently permittivity in the rock s alt. The radio wave had been reflected due to the irregularity of the perm ittivity in the rock salt. In this conference we report measurements of ph ase changes as well as amplitude changes of a radio wave reflected from no t only rock salt but also ice. A coaxial tube was filled with rock salt or ice and an open end was irradiated by the 2MeV-electron beam. We found th at the amount of the phase change was in accord with the propagation delay of the radio wave due to the increase of the permittivity in the media. T he reflection effect is expected in all dielectrics whose permittivities d epend on their temperatures. When a GZK neutrino interacts with the detect ion media\, the energy is dissipated to the location to rise the temperatu re. The radio-wave-reflection effect would be applicable to detect ultra-h igh-energy neutrinos in all kinds of detection media made of solid dielect rics with a gigantic mass and a long attenuation length for a radio wave s uch as an ice sheet at Antarctica as well as a huge rock salt dome\, and i n the future at the moon’s crust. A phased-array radar with a peak power of 1 GW (Equivalent Isotropic Radiation Power) could detect around10 GZK neutrinos per year within the fiducial mass of 50 Gt.\n\nhttp://indico.cer n.ch/contributionDisplay.py?contribId=27&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=27&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:On the microwave signal of air showers measured with CROME DTSTART;VALUE=DATE-TIME:20120621T133000Z DTEND;VALUE=DATE-TIME:20120621T135000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-20@cern.ch DESCRIPTION:Speakers: WERNER\, Felix (Karlsruhe Institute of Technology)\n Microwave radiation from high-energy air showers has been observed in the C band with the CROME setup. The properties of these showers as reconstruc ted by KASCADE-Grande will be presented. The features of the detected GHz signals will be discussed and compared with Monte Carlo predictions for di fferent emission mechanisms\, taking into account the reconstruction uncer tainties of KASCADE-Grande.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=20&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=20&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Towards Determining the energy of the UHECRs observed by the ANITA detector. DTSTART;VALUE=DATE-TIME:20120621T154000Z DTEND;VALUE=DATE-TIME:20120621T160000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-21@cern.ch DESCRIPTION:Speakers: Dr. BELOV\, Konstantin (UCLA)\nThe Antarctic Impulsi ve Transient Antenna (ANITA) is a balloon-borne radio experiment designed to discover ultra-high energy cosmic neutrinos. The ANITA detector has com pleted one prototype and two full-scale flights above the Antarctic contin ent. Two direct and fourteen reflected cosmic ray events of the ultra-high energy were observed during the first full scale flight and several other s in the second flight. We present a Monte Carlo technique and analysis de veloped to determine the energy of the primary cosmic ray particles\nfrom the ANITA data.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId= 21&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=21&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Radio emission from Air Showers. Comparison of theoretical approac hes. DTSTART;VALUE=DATE-TIME:20120622T095500Z DTEND;VALUE=DATE-TIME:20120622T101500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-22@cern.ch DESCRIPTION:Speakers: Dr. BELOV\, Konstantin (UCLA)\nWhile the fluorescenc e and the ground counter techniques of the ultra-high energy cosmic rays ( UHECR) detection were being developed for decades\, the interest in the ra dio detection diminished after the initial experiments in the 1960s. As a result\, the fluorescence and the surface array techniques are more mature today\, providing more reliable measurements of the primary cosmic partic le energy\, chemical composition and the inelastic cross-section. The adva ntages of the radio technique are 100% duty cycle and lower deployment and operational costs. Thus\, the radio technique can greatly complement the fluorescence and the ground array detection and can also work independent ly. With the ANITA balloon detector observing UHECRs and the success of LO PES\, CODALEMA and other surface radio detectors\, the radio technique got a significant boost in recent years. Reliable Monte Carlo (MC) simulation s are needed in order to obtain the energy and other parameters of the pri mary cosmic ray particle from the radio observations. Several MC technique s like\,\nZHairesS and the Endpoint Formalism\, were proposed in recent\ny ears. While they seem to reproduce some of the observed data quite\nwell\, there is a divergence between the different approaches under\ncertain con ditions. In this work we derive these approaches from\nMaxwell'’s equati ons\, discuss their similarity and limitations that\nare applicable to the UHECR air showers and to the proposed experiment at SLAC.\n\nhttp://indic o.cern.ch/contributionDisplay.py?contribId=22&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=22&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Data analysis challenges of gravitational-wave astronomy DTSTART;VALUE=DATE-TIME:20120621T070000Z DTEND;VALUE=DATE-TIME:20120621T074000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-49@cern.ch DESCRIPTION:Speakers: CHASSANDE-MOTTIN\, Eric (CNRS AstroParticule et Cosm ologie)\nGravitational waves are radiative solutions of space-time dynamic s predicted by Einstein's theory of General Relativity. A world-wide array of large-scale and highly-sensitive interferometric detectors constantly scrutinizes the geometry of the local space-time with the hope to detect d eviations that would sign an impinging gravitational wave from a remote as trophysical source. Finding the rare and weak signature of gravitational w aves buried in non-stationary and non-Gaussian instrument noise is a parti cularly challenging problem. We will give an overview of the data-analysis techniques and associated observational results obtained so far by Virgo (in Europe) and LIGO (in the US)\, alongwith the prospects offered by the up-coming advanced versions of those detectors.\n\nhttp://indico.cern.ch/c ontributionDisplay.py?contribId=49&sessionId=6&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=49&sessionId=6& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Lunar Imaging and Ionospheric Calibration for the Lunar Cherenkov Technique DTSTART;VALUE=DATE-TIME:20120619T135500Z DTEND;VALUE=DATE-TIME:20120619T141500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-47@cern.ch DESCRIPTION:Speakers: MCFADDEN\, rebecca (ASTRON)\nThe Lunar Cherenkov tec hnique is a promising method for UHE neutrino and cosmic ray detection whi ch aims to detect nanosecond radio pulses produced during particle interac tions in the Lunar regolith. For low frequency experiments\, such as NuMoo n\, the frequency dependent dispersive effect of the ionosphere is an impo rtant experimental concern as it reduces the pulse amplitude and subsequen t chances of detection. We present continuing results from a new method to calibrate the dispersive effect of the ionosphere on Lunar Cherenkov puls es via Faraday rotation measurements of the Moon’s polarised emission co mbined with geomagnetic field models. We also extend this work to include radio imaging of the Lunar surface\, which provides information on the phy sical and chemical properties of the Lunar surface that may affect experim ental strategies for the Lunar Cherenkov technique.\n\nhttp://indico.cern. ch/contributionDisplay.py?contribId=47&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=47&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Measurements of the GHz emission by a 3 MeV electron beam. DTSTART;VALUE=DATE-TIME:20120621T152000Z DTEND;VALUE=DATE-TIME:20120621T154000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-44@cern.ch DESCRIPTION:Speakers: FACAL SAN LUIS\, Pedro (University of Chicago)\nThe MAYBE (Microwave Air Yield Beam) Experiment is dedicated to the study of t he microwave emission from particle beams in the light of its possible us e in the detection of ultra high energy cosmic rays.\nMeasurements of the microwave emission from an electron-beam where performed at the 3 MeV elec tron Van de Graaff facility of the Argonne National Laboratory. Results i nclude the measured spectrum between 1 and 15 GHz\, the polarization\, and the scaling of the power with respect to the beam intensity. MAYBE measur ements provide further insight on microwave emission as a detection techni que for ultra-high energy cosmic rays.\n\nhttp://indico.cern.ch/contributi onDisplay.py?contribId=44&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=44&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Compact array calibrator for UHE neutrino acoustic detection DTSTART;VALUE=DATE-TIME:20120621T080000Z DTEND;VALUE=DATE-TIME:20120621T082000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-29@cern.ch DESCRIPTION:Speakers: Ms. ADRIÁN-MARTÍNEZ\, Silvia (UPV)\nIn situ acoust ic calibration devices should play a very important role to assure the rig ht performance of sensors and detectors for the acoustic detection of ultr a-high energy neutrinos in underwater telescopes. Moreover\, they provide evidences for the feasibility evaluation of the technique and for the effi ciency determination of the entire detector. Following previous studies\, relating with parametric acoustic generation\, a first prototype of a comp act acoustic array able to mimic the acoustic neutrino signal (a very dire ctive transient bipolar signal with ‘pancake’ directivity) is presente d. The compact array developed has practical features such as easy handlin g\, operation and versatile functionality. The transmitter is able to work in different frequency ranges\, for different application modes\, being p ossible to carry out several tasks related with acoustics in underwater ne utrino telescopes: emission of neutrino-like signals\, calibration of sens or sensitivities and responses\, emission of signals for positioning\, etc . The design\, construction and characterization of the prototype are desc ribed. A propagation simulation study of experimental signals over km dist ances is also discussed.\n\nhttp://indico.cern.ch/contributionDisplay.py?c ontribId=29&sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=29&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Simulation Chain for Acoustic Ultra-high Energy Neutrino Detectors in Water DTSTART;VALUE=DATE-TIME:20120621T095500Z DTEND;VALUE=DATE-TIME:20120621T101500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-40@cern.ch DESCRIPTION:Speakers: Mr. NEFF\, Max (ECAP - Uni Erlangen)\nAcoustic neutr ino detection is a promising approach for large-scale ultra-high energy ne utrino detectors in water. In this contribution\, a Monte Carlo simulation chain for acoustic neutrino detection devices in water will be presented. The simulation chain covers the generation of the acoustic pulse produced by a neutrino interaction and its propagation to the sensors within the d etector. Currently\, ambient and transient noise models for the Mediterran ean Sea and simulations of the data acquisition hardware\, similar to the one used in ANTARES/AMADEUS\, are implemented. A pre-selection scheme for neutrino-like signals based on matched filtering is employed\, as it can b e used for on-line filtering. To simulate the whole processing chain for e xperimental data\, signal classification and acoustic source reconstructio n algorithms are integrated. An overview of the design and capabilities of the simulation chain will be presented\, and some applications and prelim inary studies will be discussed.\n\nhttp://indico.cern.ch/contributionDisp lay.py?contribId=40&sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=40&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:LUNASKA neutrino search with the Parkes and ATCA telescopes DTSTART;VALUE=DATE-TIME:20120619T131000Z DTEND;VALUE=DATE-TIME:20120619T133500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-41@cern.ch DESCRIPTION:Speakers: Mr. BRAY\, Justin (University of Adelaide)\nThe Moon is used as a target volume for ultra-high energy neutrino searches with t errestrial radio telescopes. The LUNASKA project has conducted observatio ns with the Parkes and ATCA telescopes\; and\, most recently\, with both o f them in combination. We present an analysis of the data obtained from t hese searches\, including validation and calibration results for the Parke s-ATCA experiment\, as well as a summary of prospects for future observati ons.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=41&sessionI d=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=41&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Detecting Radio Emission from Cosmic Rays with LOFAR DTSTART;VALUE=DATE-TIME:20120622T074000Z DTEND;VALUE=DATE-TIME:20120622T080500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-0@cern.ch DESCRIPTION:Speakers: NELLES\, Anna (Radboud University Nijmegen)\nLOFAR ( the Low Frequency Array) is the largest radio telescope in the world for o bserving low frequency radio emission from 10 to 240 MHz. In addition to i ts use as an interferometric array\, LOFAR is now routinely used to detect cosmic ray induced air showers by their radio emission.\n\nThe LOFAR core in the Netherlands has a higher density of antennas than any other dedica ted cosmic ray experiment. On an area of nearly 5 km^2 about 1800 antennas are installed. They measure the radio emission from air showers with unpr ecedented precision and\, therefore\, give the perfect opportunity to dise ntangle the physical processes which cause the radio emission in air showe rs. In parallel to ongoing astronomical observations LOFAR is triggered by a particle detector (LORA) to record the time series containing the cosmi c ray pulses. \n\nCosmic rays have been measured with LOFAR since June 201 1. We will present the results of the first year of data. Special emphasis will be put on the reconstruction chain and the lateral signal distributi on.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=0&sessionId= 7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=0&sessionId=7&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:In situ study of efficiency and angular coverage of acoustic senso rs of the South Pole Acoustic Test Setup DTSTART;VALUE=DATE-TIME:20120621T074000Z DTEND;VALUE=DATE-TIME:20120621T080000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-3@cern.ch DESCRIPTION:Speakers: NAHNHAUER\, Rolf (DESY)\nThe South Pole Acoustic Tes t Setup (SPATS) consists of four strings\,\n each instrumented with seven acoustic sensors and transmitters frozen\nin the upper 500 m of IceCube ho les. SPATS sensors have been extensively studied in the laboratory at chan ging temperatures and pressure in air\, water and ice. It was however impo ssible to create conditions like in deep ice at the South Pole. We present here different methods to investigate angular coverage and efficiency of the acoustic sensors after deployment. The corresponding results are used to discuss the reliability of SPATS detector measurements. We conclude wit h an outlook about the applicability of the described methods to future ac oustic or hybrid detectors for cosmogenic neutrino measurements in ice.\n\ nhttp://indico.cern.ch/contributionDisplay.py?contribId=3&sessionId=8&conf Id=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=3&sessionId=8&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Tunka-Rex: a Radio Antenna Array for the Tunka Experiment DTSTART;VALUE=DATE-TIME:20120622T080500Z DTEND;VALUE=DATE-TIME:20120622T082500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-5@cern.ch DESCRIPTION:Speakers: SCHRÖDER\, Frank (Karlsruhe Institute of Technology (KIT))\nTunka-Rex (Tunka radio extension) will be an array of about 20 an tennas at the Tunka experiment close to Lake Baikal in Siberia. The antenn as will be connected directly to the data acquisition of the Tunka main de tector\, a 1 km² large array of 133 non-imaging photomultipliers observin g the Cherenkov light of air showers in dark and clear nights. This allows to cross-calibrate the radio signal with the Cherenkov signal of the same air showers - in particular with respect to the energy and the atmospheri c depth of the shower maximum\, Xmax. Consequently\, theoretical predictio ns can be tested whether in rural regions with low radio background the ra dio precision comes indeed close to the precision of the established fluor escence and air-Cherenkov techniques. At a mid-term perspective\, due to i ts higher duty-cycle\, Tunka-Rex can then enhance the effective observing time of Tunka by an order of magnitude\, at least in the interesting energ y range above 100 PeV. Moreover\, Tunka-Rex is very cost-effective\, e.g.\ , by using economic Short Aperiodic Loaded Loop Antennas (SALLAs). Thus\, the results of Tunka-Rex and the comparison to other sophisticated radio a rrays will provide crucial input for future large-scale cosmic-ray observa tories\, for which measurement precision as well as costs per area have to be optimized.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=5 &sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=5&sessionId=7&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Measurements with LOPES: Status and Recent Results DTSTART;VALUE=DATE-TIME:20120620T150000Z DTEND;VALUE=DATE-TIME:20120620T152500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-4@cern.ch DESCRIPTION:Speakers: SCHRÖDER\, Frank (Karlsruhe Institute of Technology (KIT))\nLOPES is a digital antenna array at the Karlsruhe Institute of Te chnology\, Germany\, for cosmic-ray air-shower measurements. Triggered by the co-located KASCADE-Grande air-shower array\, LOPES detects the radio e mission of air showers via digital radio interferometry. We will summarize the status of LOPES and recent results concerning the understanding of th e radio emission and the reconstruction of air-shower properties from the radio signal. We will present an update of results on the successful recon struction of energy and arrival direction of the primary particles. Even m ore important for many particle and astrophysics questions is the reconstr uction of the atmospheric depth of the shower maximum\, Xmax\, which yield s information on the type of the primary particle and its interaction with the atmosphere. We found experimental evidence that radio measurements ar e indeed sensitive to the longitudinal development of air showers\, since we observe a correlation between the slope of radio-lateral distributions and measurements of the muon-tracking detector of KASCADE-Grande. Moreover \, since recently improved REAS simulations come close to the measurements \, they are used as input for the reconstruction of Xmax. Unfortunately\, at LOPES\, the Xmax precision is limited by the high level of anthropogeni c radio background\, but the developed methods can be\ntransferred to next generation experiments with lower background.\n\nhttp://indico.cern.ch/co ntributionDisplay.py?contribId=4&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=4&sessionId=7&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Acoustic positioning system in ice for the Enceladus Explorer DTSTART;VALUE=DATE-TIME:20120620T084000Z DTEND;VALUE=DATE-TIME:20120620T090000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-7@cern.ch DESCRIPTION:Speakers: HOFFMANN\, Ruth (Bergische Universität Wuppertal)\n The IceMole\, a combination of melting and drilling probe\, which is able to move and steer through ice and take samples while doing so\, can be use d to install instruments in ice. An improved design of the prototype devel oped by the FH Aachen\, the Eceladus Explorer\, could be used to explore w ater filled cracks on the Saturn moon Enceladus some day. Before starting a space mission to Enceladus the next step will be the exploration of the Taylor Glacier in the Antarctica. The probe will operate in this similar\, smaller scale scenario in order to test the functionality of itself and i ts inner systems. The icecraft will be equipped in addition to an inertial navigation system with an acoustic positioning system. The acoustic syste m\, composed of receivers in the probe itself and several emitters (pinger ) on the glacier surface\, will determine the position of the IceMole by m easuring the signal propagation time and triangulation\, which requires a solid knowledge of the propagation of acoustic signals in ice. Especially the characteristics of this glacier ice\, such as the speed of sound and t he acoustic attenuation length\, which depend on the density and temperatu re of the ice\, have to be known. A method to determine these properties d uring the operation of the IceMole will be developed.\nIn this talk we wil l give an overview over the project. We will present the status of the dev elopment of the acoustic surface system and we will show the results of fi rst measurements in glacier ice.\n\nhttp://indico.cern.ch/contributionDisp lay.py?contribId=7&sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=7&sessionId=8&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Acoustic Neutrino Detection in Ice: Past\, Present and Future DTSTART;VALUE=DATE-TIME:20120620T074000Z DTEND;VALUE=DATE-TIME:20120620T082000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-6@cern.ch DESCRIPTION:Speakers: KARG\, Timo ()\nAcoustic neutrino detection is a pro mising technique to instrument the large volumes required to measure the s mall expected flux of ultra-high energy cosmogenic neutrinos. Using ice as detection medium allows for coincident detection of neutrino interactions with acoustic sensors\, radio antennas and optical light sensors with the benefit of cross calibration possibilities or independent measurements of the the same event. We will review the past development of the field and discuss its current status and challenges. Results from site exploration s tudies\, mainly by the South Pole Acoustic Test Setup (SPATS) which has be en codeployed with the IceCube neutrino telescope at South Pole\, and curr ent physics results will be presented. Current ideas for the design\, cali bration\, and deployment of acoustic sensors for new projects will be show n. The possible role of the acoustic technique in future in-ice neutrino d etectors will be discussed.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=6&sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=6&sessionId=8&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Performance of the Aachen Acoustic Laboratory and results from com parative studies in water and ice. DTSTART;VALUE=DATE-TIME:20120621T084000Z DTEND;VALUE=DATE-TIME:20120621T090000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-9@cern.ch DESCRIPTION:Speakers: HEINEN\, Dirk (R)\nTo investigate acoustic ice prope rties under laboratory conditions and to test the thermo-acoustic model\, the Aachen Acoustic Laboratory (AAL) was founded as a part of the acoustic working group (SPATS) within the IceCube collaboration. \nThe AAL provide s a test facility setup with a proper infrastructure to study acoustics an d thermo-acoustics in a large volume of water and ice. The control on the freezing process\, the ice quality\, the temperature monitoring at differe nt phases of the medium and the laser-based thermo-acoustic sound generati on are the key ingredient of the setup. \nThe AAL setup provides the possi bility for the characterization of a wide range of acoustic transducer\, s ensor/transmitter calibration\, study of the thermo-acoustic sound generat ion\, study of the acoustic properties of the ice\, water as well as the w ater/ice interfaces\, and R&D of new types of acoustic transducers (PVDF-b ased) as an alternative to standard PZTs.\nIn this document the different parts of the AAL setup are described\,\nresults on the commissioning of th e laser based thermo-acoustic sound generation are presented and the perfo rmance of the absolute sensor calibration method in water and ice is discu ssed.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=9&sessionI d=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=9&sessionId=8&c onfId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Ultra High Frequency Geomagnetic Radiation from Extensive Air Show ers DTSTART;VALUE=DATE-TIME:20120620T141000Z DTEND;VALUE=DATE-TIME:20120620T143000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-18@cern.ch DESCRIPTION:Speakers: Dr. CARVALHO JR.\, Washington (University of Santiag o de Compostela)\nUsing the ZHAireS Monte Carlo code\, we show that the F ourier-spectrum of the radio emission of inclined air showers can have a s izable intensity up to the GHz frequency range. At these frequencies\, onl y the fraction of shower development seen at an angle close to the Cherenk ov angle contributes to the observable emission\, which is mainly due to t he geomagnetic and charge excess mechanisms. At ground level\, the maximu m emission at high frequencies is concentrated in an elliptical region rel ated to the intersection with ground of a Cherenkov cone with origin clos e to shower maximum. Moreover\, the lateral distribution of the signal at ground contains information on the shower longitudinal profile. In this wo rk we characterize this effect which can be very important for ground-base d radio experiments aiming at detecting molecular bremsstrahlung radiation in the GHz range - a different mechanism not included in ZHAireS simulati ons. We also show that the simulated spectrum is consistent with the pulse s detected by ANITA attributed to radio emission from UHECRs.\n\nhttp://in dico.cern.ch/contributionDisplay.py?contribId=18&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=18&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Electromagnetic radiation in the Tamm problem DTSTART;VALUE=DATE-TIME:20120622T093500Z DTEND;VALUE=DATE-TIME:20120622T095500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-39@cern.ch DESCRIPTION:Speakers: JAMES\, Clancy (University of Erlangen-Nuernberg)\nT he 'Tamm Problem' (Tamm\, 1939) is the calculation of the electromagnetic radiation emitted by a particle travelling a finite distance at a uniform (relativistic) velocity in a medium. It is exactly the problem which needs to be solved in Monte-Carlo simulations of the radio-emission from indivi dual particles. The two main formulas used in calculations - the ZHS algor ithm and the endpoint formulation - both use approximations in their deriv ations\, the effect of which in realistic problems is currently unclear.\n \nIn this contribution\, the ZHS and endpoint solutions to the Tamm proble m are compared using simple toy experiments. In order to resolve questions on each method's accuracy\, a new approach to the problem is presented\, which attempts to make none of the assumptions inherent in these previous formulas. The applicability of the ZHS and endpoint approaches is then re- assessed in light of this information.\n\nhttp://indico.cern.ch/contributi onDisplay.py?contribId=39&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=39&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Energy Estimation for Cosmic Rays Measured with the Auger Engineer ing Radio Array DTSTART;VALUE=DATE-TIME:20120619T160500Z DTEND;VALUE=DATE-TIME:20120619T162500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-38@cern.ch DESCRIPTION:Speakers: Mr. GLASER\, Christian (RWTH Aachen)\nThe Auger Engi neering Radio Array (AERA) is located within the Pierre-Auger Observatory and currently consists of 24 self-triggered radio stations. Observation of radio signals from cosmic rays is confirmed by the surface detector (SD) stations of the observatory which provide well calibrated information on t he cosmic ray energies and arrival directions. The response of the radio s tations has been thoroughly calibrated to enable reconstruction of the inc oming electric field. For estimating the cosmic ray energy we use the maxi mum absolute value of the measured electric field vector corrected for the incoming direction and the distance to the shower core. Performing an ene rgy calibration using the SD information we observe that the defined radio energy estimator provides an approximately linear dependency on the cosmi c ray energy.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=38 &sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=38&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Comparison of LOPES measurements with CoREAS and REAS 3.1 simulati ons DTSTART;VALUE=DATE-TIME:20120620T152500Z DTEND;VALUE=DATE-TIME:20120620T154500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-14@cern.ch DESCRIPTION:Speakers: Dr. LUDWIG\, Marianne (Karlsruhe Institute of Techno logy)\nIn the previous years\, LOPES emerged as a very successful experime nt measuring the radio emission from air showers in the MHz frequency ran ge. In parallel\, the theoretical description of radio emission was develo ped further and REAS 3.1 became a well-respected simulation Monte Carlo co de. REAS 3.1 as well as CoREAS are based on the endpoint formalism\, i.e. no assumptions on the emission mechanism have to be made. While REAS 3.1 i s based on histograms derived from CORSIKA simulations\, CoREAS is directl y implemented into CORSIKA without beeing affected by possible lost of inf ormation due to histogramming the particle distributions. In the newest ve rsions of REAS and CoREAS\, a realistic atmospheric refractive index is co nsidered.\nTo improve the understanding of the emission processes and judg e the quality of CoREAS and REAS 3.1\, we compare the theoretical predicti ons of both codes with high-quality events measured by LOPES. We present r esults concerning the lateral distribution and the absolute amplitude at a typical distance to the shower axis of the radio signal. Moreover\, we co mpare the dependence of the amplitude and the slope parameter of the later al distribution function with shower parameters.\n\nhttp://indico.cern.ch/ contributionDisplay.py?contribId=14&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=14&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Simulating radio emission from air showers with CoREAS DTSTART;VALUE=DATE-TIME:20120620T131000Z DTEND;VALUE=DATE-TIME:20120620T133000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-11@cern.ch DESCRIPTION:Speakers: Dr. HUEGE\, Tim (Karlsruhe Institute of Technology)\ nIn the Monte Carlo simulation code REAS\, radio emission from air showers is calculated using the "endpoint formalism". No assumptions on the emiss ion mechanism have to be made in this parameter-free approach.\n\nREAS sim ulations are based on particle distributions which have been simulated wit h CORSIKA and then exported as 4-dimensional histograms. During the histog ramming\, however\, information is lost. For example\, the geomagnetically induced dipole moment of the electron-positron distribution is not conser ved\, and the preferred outward drift of secondary particles is not reflec ted in the histogrammed distributions either.\n\nFor an even more precise simulation of the radio emission\, we have thus implemented the endpoint f ormalism directly into CORSIKA. This new simulation code\, named CoREAS\, takes into account the full complexity of air shower physics without any a pproximations. In this presentation we will describe the concept and imple mentation of CoREAS and present simulation results including realistic ref ractive index effects in the atmosphere.\n\nhttp://indico.cern.ch/contribu tionDisplay.py?contribId=11&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=11&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Spectral index analysis of the data from the Auger Engineering Rad io Array DTSTART;VALUE=DATE-TIME:20120619T162500Z DTEND;VALUE=DATE-TIME:20120619T164500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-10@cern.ch DESCRIPTION:Speakers: GREBE\, Stefan (Radboud University Nijmegen)\nThe fi rst stage of the Auger Engineering Radio Array has been deployed at the Pi erre Auger Observatory in Argentina and is taking data. It measures radio signals in the MHz range from air showers induced by cosmic rays with ener gies above 10^17 eV. It is overlooked by the fluorescence telescopes and i s located in a dense part of the particle detector array. This allows for cross-calibration of the individual techniques and therefore this is an ex cellent location to study radio emission from extensive air showers.\nThe index of the measured frequency spectra of the cosmic-ray-induced signals changes with the distance of the detector to the shower axis and with the zenith angle. The observed dependencies are in agreement with simulations. We are investigating whether the spectral index can be used as a tool to determine the composition of cosmic rays.\n\nhttp://indico.cern.ch/contrib utionDisplay.py?contribId=10&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=10&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:First results from EVA simulations\; Cherenkov effects and the che mical composition of the initial cosmic ray. DTSTART;VALUE=DATE-TIME:20120620T135000Z DTEND;VALUE=DATE-TIME:20120620T141000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-13@cern.ch DESCRIPTION:Speakers: SCHOLTEN\, Olaf (KVI/University of Groningen)\nWe di scuss the first results of macroscopic calculations based on full Monte-Ca rlo simulations including a realistic index of refraction using the EVA-co de. Due to the finite refractivity Cherenkov effects play an important rol e in radio emission from air showers. We show that the observed frequency spectrum depends strongly on the distance from the shower core. At the Che renkov angle the high frequency components have the largest power. It foll ows that the Lateral Distribution Function of the radio emission can be us ed as an excellent probe to determine the shower maximum and thus give a h andle on the chemical composition of the initial cosmic ray. Furthermore\, we show how Cherenkov effects affect the two main emission mechanisms\, t he geomagnetic emission and the charge-excess emission.\n\nhttp://indico.c ern.ch/contributionDisplay.py?contribId=13&sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=13&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:The EVA code\; Macroscopic modeling of radio emission from air sho wers based on full MC simulations including a realistic index of refractio n. DTSTART;VALUE=DATE-TIME:20120620T133000Z DTEND;VALUE=DATE-TIME:20120620T135000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-12@cern.ch DESCRIPTION:Speakers: DE VRIES\, Krijn D. (KVI/University of Groningen)\nA comprehensive overview of the newly developed EVA-code will be given by m aking a direct comparison to the MGMR-code. Both codes perform a macroscop ic calculation of radio emission from cosmic-ray-induced air showers. The MGMR-model is based on parameterized shower distributions ignoring the lat eral extend of the shower. Furthermore\, all calculations ignored Cherenko v effects. To take into account Cherenkov effects and include realistic sh owers in combination with shower-to-shower fluctuations we have developed the EVA-code (Electric fields\, using a Variable index of refraction in Ai r shower simulations code). The EVA-code is a full Monte-Carlo simulation for radio emission from cosmic-ray-induced air showers. The EVA-code makes use of the finite dimensions of the particle distributions to overcome th e divergences in the fields due to Cherenkov effects without making any ap proximations.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=12 &sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=12&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Overview of MHz air shower radio experiments and results DTSTART;VALUE=DATE-TIME:20120619T150000Z DTEND;VALUE=DATE-TIME:20120619T154000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-58@cern.ch DESCRIPTION:Speakers: REVENU\, Benoît (CNRS/IN2P3)\nAfter 10 years of eff orts\, important progress have been made in the field of radio-detection o f extensive air showers in the MHz range. The geomagnetic contribution has been proven to be dominant. A secondary process in the shower (probably r elated to the excess of charges in the shower) has also been detected. The correlation between the detected electric field and the nature and energy of the primary cosmic ray is on the way to be established through both si mulation and data. I will present the main experiments in this field and r eview their main results.\n\nhttp://indico.cern.ch/contributionDisplay.py? contribId=58&sessionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=58&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Lunar Space Missions for Observation of Ultrahigh-Energy Cosmic Ra ys and Neutrinos DTSTART;VALUE=DATE-TIME:20120619T141500Z DTEND;VALUE=DATE-TIME:20120619T143500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-16@cern.ch DESCRIPTION:Speakers: Dr. GUSEV\, German (Lebedev physical institute)\nTwo stages of a lunar experiment with the regolith as a target for the intera ction of ultrahigh-energy cosmic rays and neutrinos are described. The fir st stage deals with the LORD experiment within the framework of the Luna-G lob space mission scheduled for the nearest future. The current status of the LORD-instrumentation development is discussed. The aperture of the lun ar orbital radio detector exceeds all existing ground-based arrays. Succes sful realization of the LORD experiment will make it possible to start the second stage of the program. Multi-satellite lunar orbital systems are pr oposed to increase the measurement statistics and accuracy.\n\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=16&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=16&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Ultra-high energy cosmic neutrinos with the IceCube neu trino observatory. DTSTART;VALUE=DATE-TIME:20120621T101500Z DTEND;VALUE=DATE-TIME:20120621T105500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-33@cern.ch DESCRIPTION:Speakers: YOSHIDA\, Shigeru (Chiba University)\nWe review the present status of the search for ultra-high energy cosmic neutrinos with t he conventional methods. The IceCube neutrino observatory has currently re alised the best sensitivity on detection of neutrinos in the energy range around EeV\, by the standard neutrino detection technique measuring ultra- violet Cherenkov light emissions. The most updated results from the data o btained by the increased instrumentation volume of the IceCube optical sen sor array are reported\, followed by discussions on its implication to ori gin of ultra-high energy cosmic rays. The another conventional technique u sing deeply penetrating airshowers also provides a capability to search fo r ultra-high energy neutrinos by a giant cosmic ray airshower detector. We briefly mention the published results obtained by the Pierre Auger observ atory and the future outlook by the planned JEM-EUSO mission.\n\nhttp://in dico.cern.ch/contributionDisplay.py?contribId=33&sessionId=6&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=33&sessionId=6& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:A Linear Array Hydrophone Transmitter for the calibration of acou stic UHE Neutrino Telescopes DTSTART;VALUE=DATE-TIME:20120621T082000Z DTEND;VALUE=DATE-TIME:20120621T084000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-32@cern.ch DESCRIPTION:Speakers: DANAHER\, sean (N)\nThe calibration and design of an eighth hydrophone linear array has been developed for the generation of e mulated Ultra High Energy (UHE) neutrino-induced pulses. This acoustic ar ray simulates the acoustic pulse created from a UHE neutrino interaction i n water by generating a coherently emitted acoustic bipolar pulse. The cal ibrator is developed using signal processing methods using experimental me asurements to characterise the hydrophone system. An 8 channel PIC hydroph one array module has been built for processing and control. A linear array simulation for the neutrino pulses production has been studied in order t o predict the directivity and shape of the acoustic bipolar pulse at the A NTARES neutrino detector. The calibrator was deployed above the ANTARES s ite in September 2011. The result of the analysis of the first sea campaig n over ANTARES will be presented.\n\nKeywords: Array hydrophone calibratio n\; UHE neutrinos\;\nAcoustic detection\; PIC module\; array simulation.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=32&sessionId=8&co nfId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=32&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Prospects for an air-shower radio extension to IceCube DTSTART;VALUE=DATE-TIME:20120622T082500Z DTEND;VALUE=DATE-TIME:20120622T084500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-31@cern.ch DESCRIPTION:Speakers: BOESER\, Sebastian (U)\nWith its 1km3 in-ice sensor array complemented by a 1km2 surface array of ice-Cherenkov tanks for part icle detection\, the IceCube observatory is not only the largest neutrino telescope but also one of the world's most competitive instrument for stud ying cosmic rays in the PeV to EeV regime. In particular\, studying high-e nergy muons from\nthe shower core in coincidence with particle flux on the surface yields a handle on cosmic ray composition in the energy range whe re the transition from galactic to extra-galactic sources should occur.\n\ nFurther augmenting the IceCube observatory with an array of radio sensor in the 10-100MHz regime will additionally allow for observation of the geo magnetic radio emission from the air shower. Reflecting the whole shower d evelopment\, this radio signal will not only provide for significantly red ucing the systematic errors involved with the sampling approaches\, but wi ll also result in an additional\, independent handle on the shower maximum . Such a triple-technology array should therefore significantly improve th e understanding of cosmic rays.\n\nI will present first results from explo ratory instrumentation deployed at the SouthPole\, indicating its suitabil ity for this approach. In addition\, first performance studies using a det ailed MonteCarlo simulation including IceCube/IceTop and the radio array w ill be shown\, and prospects for the installation of a test array will be discussed.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=31&se ssionId=7&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=31&sessionId=7& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Radio Detection in Dense Matter: Balloon\, telescope\, satellite DTSTART;VALUE=DATE-TIME:20120619T123000Z DTEND;VALUE=DATE-TIME:20120619T131000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-56@cern.ch DESCRIPTION:Speakers: SECKEL\, David (University of Delaware)\nRadio Detec tion in Dense Matter: Balloon\, telescope\, satellite\n\nhttp://indico.cer n.ch/contributionDisplay.py?contribId=56&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=56&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Towards high energy neutrino acoustic detector in Lake Baikal: cur rent status and perspectives. DTSTART;VALUE=DATE-TIME:20120621T093000Z DTEND;VALUE=DATE-TIME:20120621T095500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-37@cern.ch DESCRIPTION:Speakers: Prof. BUDNEV\, Nikolay (Irkutsk State University)\nW e report the present status and perspectives of the feasibility study to d etect cosmic neutrinos acoustically in Lake Baikal. The results of a backg round studies are presented. It was shown that most of the detected backgr ound neutrino-like pulses come from the lake surface. This fact has been u sed in project of an acoustic prototype detector that consists of compact modules with 4-channel antennas each\, arranged above the Baikal Neutrino Telescope at shallow depths and "listens" the deep-water layers of the la ke. The results of test experiments and of data taking with the detector a re presented.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=37 &sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=37&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Combined Opto-Acoustical Sensor Modules for KM3NeT DTSTART;VALUE=DATE-TIME:20120620T082000Z DTEND;VALUE=DATE-TIME:20120620T084000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-36@cern.ch DESCRIPTION:Speakers: ENZENHÖFER\, Alexander (ANTARES)\nThe use of acoust ical sensors in combination with optical sensors within one sensor module is a promising alternative to the standard design of deep-sea neutrino tel escopes with separate acoustical and optical devices. These so-called Opto -Acoustical Modules comprise at least one sensor of each type inside the s ame glass housing. In this combination it is possible to determine the mod ule position and orientation by acoustical triangulation without the need for additional external receivers. An adapted data readout scheme with cus tom-designed acoustical sensors also allows for extended analysis objectiv es like deep-sea observations or acoustical particle detection. The electr o-magnetic interference of the different sensors within a module is the ma in challenge for the feasibility of Opto-Acoustical Modules. Prototypes wi th different geometrical arrangements and numbers of sensors have to be st udied in order to demonstrate and optimise the overall applicability of th ese modules.\n\nThis presentation describes first results obtained for two different designs measured in different laboratories.\n\nhttp://indico.ce rn.ch/contributionDisplay.py?contribId=36&sessionId=8&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=36&sessionId=8& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Simulation of radio emission from cosmic ray air shower with SELFA S2 DTSTART;VALUE=DATE-TIME:20120621T160000Z DTEND;VALUE=DATE-TIME:20120621T162000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-35@cern.ch DESCRIPTION:Speakers: MARIN\, Vincent (Subatech)\nWe present a microscopic computation of the radio emission from air showers initiated by ultra-hig h energy cosmic rays in the atmosphere. The strategy adopted is to compute each secondary particle contribution of the electromagnetic component and to construct the total signal at any location. SELFAS2 is a code which do esn’t rely on air shower generators like AIRES or CORSIKA and it is base d on the concept of air shower uni- versality which makes it completely au tonomous. Each positrons and electrons of the air shower are generated ran domly following relevant distributions and tracking them along their trave l in the atmosphere. We show in this paper that the radio emission is main ly due to the time derivative of the transverse current and the time deriv ative of the charge excess (see also [1]). The time derivative of the tran sverse current created by systematic deviations of charges in the geomagne tic field is usually dominant compared to the charge excess contribution e xcept for the case of an air shower parallel to the geomagnetic field.\n\n http://indico.cern.ch/contributionDisplay.py?contribId=35&sessionId=9&conf Id=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=35&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Ground Based Radio Detection in Dense Matter DTSTART;VALUE=DATE-TIME:20120620T093000Z DTEND;VALUE=DATE-TIME:20120620T101000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-52@cern.ch DESCRIPTION:Speakers: BESSON\, dave (K)\, LAHMANN\, Robert (Friedrich-Alex ander-Univ. Erlangen (DE))\nWe report on experimental efforts (ARA\, ARIAN NA\, etc) which seek neutrino detection using englacial radio receivers. B y exploiting the Askaryan effect\, such embedded sensors can achieve detec tion thresholds of order 100 PeV\, and thereby attain excellent sensitivit y to the expected cosmogenic neutrino flux. Current status\, comparison of existing experiments and future prospects will be reviewed.\n\nhttp://ind ico.cern.ch/contributionDisplay.py?contribId=52&sessionId=1&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=52&sessionId=1& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-Ray Observation via Microwave Emission (CROME) DTSTART;VALUE=DATE-TIME:20120621T131000Z DTEND;VALUE=DATE-TIME:20120621T133000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-19@cern.ch DESCRIPTION:Speakers: SMIDA\, Radomir (Karlsruhe Institute of Technology)\ nThe CROME experiment is a new setup to study microwave radiation from air showers. The GHz radiation is measured with several parabolic antennas\, each equipped with a multiple-receiver camera operating in the extended C band (3.4--4.2 GHz). Data are taken in coincidence with cosmic-ray showers detected by the KASCADE-Grande experiment. The overall experimental setup will be presented and different methods used for determining sensitivity\ , pointing\, and time synchronization of the detectors will be discussed. It is shown that the CROME setup is well-suited for the detection of pulse s of a few nanoseconds as expected from cosmic-ray showers. An overview of the first detected air shower events is given.\n\nhttp://indico.cern.ch/c ontributionDisplay.py?contribId=19&sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=19&sessionId=10 &confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:The cosmic triad: cosmic rays\, gamma-rays and neutrinos DTSTART;VALUE=DATE-TIME:20120622T070000Z DTEND;VALUE=DATE-TIME:20120622T074000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-55@cern.ch DESCRIPTION:Speakers: AHLERS\, Markus ()\nThe existence of ultra-high ener gy (UHE) cosmic-rays (CRs) is a strong motivation for neutrino astronomy a t very high energies\; it seems unavoidable that UHE CRs undergo hadronic interactions with radiation backgrounds or matter prior to their arrival a t Earth. Mesons produced in these interactions quickly decay and release a flux of high-energy neutrinos and gamma-rays. Neutrino observatories have long been searching for the faint neutrino signals from extra-galactic so urces that are smoking-gun signals of these hadronic interactions - so far without success. I will try to put this into perspective. What can we lea rn from this non-observation about candidate sources of UHE CRs? And what can we expect to see in the future?\n\nhttp://indico.cern.ch/contributionD isplay.py?contribId=55&sessionId=6&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=55&sessionId=6& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:A semi-analytic treatment of radio emission from air showers DTSTART;VALUE=DATE-TIME:20120622T091500Z DTEND;VALUE=DATE-TIME:20120622T093500Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-48@cern.ch DESCRIPTION:Speakers: SECKEL\, David (University of Delaware)\nA fast semi -analytic frequency domain calculation for the radio emission from cosmic ray air showers is presented. The shower is treated as a smooth macroscopi c current source\, separable in cartesian "shower"-coordinates\, which fac ilitates calculation of phase coherence at a remote detector. Time delays account for geometry and varying index of refraction along the shower prof ile. Current distributions are described as the product of longitudinal\, transverse\, and shower thickness profiles\, with additional parameters to account for creation of charge excess\, and transverse currents due to mu ltiple soft coulomb scattering and magnetic deflections. Comparisons are m ade to REAS 3.0\, without index of refraction\, and to COREAS with index o f refraction.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=48 &sessionId=9&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=48&sessionId=9& confId=159364 END:VEVENT BEGIN:VEVENT SUMMARY:GHz detection activities for air showers: Experiments\, accelerato r measurements\, theory DTSTART;VALUE=DATE-TIME:20120621T123000Z DTEND;VALUE=DATE-TIME:20120621T131000Z DTSTAMP;VALUE=DATE-TIME:20130523T091259Z UID:indico-contribution-159364-57@cern.ch DESCRIPTION:Speakers: Dr. ENGEL\, Ralph (Forschungszentrum Karlsruhe)\nGHz detection activities for air showers: Experiments\, accelerator measureme nts\, theory\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=57& sessionId=10&confId=159364 LOCATION:Erlangen Castle (centre of town) URL:http://indico.cern.ch/contributionDisplay.py?contribId=57&sessionId=10 &confId=159364 END:VEVENT END:VCALENDAR