BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Askaryan Radio Array (ARA): Status and Performance DTSTART:20140612T123000Z DTEND:20140612T130000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3926@events.icecube.wisc.edu DESCRIPTION:Speakers: Carl Pfendner (Ohio State University)\, Eugene Hong (Ohio State University)\, Amy Connolly (Ohio State University)\n\nThe Aska ryan Radio Array (ARA) is an ultra-high energy (UHE) cosmic neutrino detec tor located at the South Pole. The cosmic ray flux cut off above primary e nergies of 10^19.5 eV leads us to expect a UHE neutrino flux due to the GZ K effect. The detection of these UHE cosmic neutrinos will add to the unde rstanding of the sources and physics of UHE cosmic rays. \n\nARA uses the radio Cherenkov technique to search for UHE neutrinos by deploying radio f requency (RF) antennas at 200m depth in the Antarctic ice and searching fo r impulsive RF signals. A prototype ARA Testbed station was deployed in th e 2010-2011 season and the first design-level ARA stations were deployed i n the 2011-2012 and 2012-2013 seasons. \n\nThree independent analysis meth ods have been developed in the search for UHE neutrinos with ARA. I will p resent the results of these first neutrino searches with 2011-2012 ARA Tes tbed data. I will also present the preliminary efforts of the extension of these methods to the analysis of the design-level stations.\n\nhttps://ev ents.icecube.wisc.edu/event/55/contributions/3926/ URL:https://events.icecube.wisc.edu/event/55/contributions/3926/ END:VEVENT BEGIN:VEVENT SUMMARY:Status and Recent Results of the Acoustic Neutrino Detection Test System AMADEUS of ANTARES DTSTART:20140609T151500Z DTEND:20140609T154000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3927@events.icecube.wisc.edu DESCRIPTION:Speakers: Robert Lahmann (Erlangen Centre for Astroparticle Ph ysics)\n\nThe technique of acoustic neutrino detection is a promising appr oach for future large-scale ultra-high-energy neutrino detectors in water. To investigate this technique in the deep sea\, the AMADEUS system has be en integrated into the ANTARES neutrino telescope in the Mediterranean Sea . Installed at a depth of more than 2000m\, the 36 acoustic sensors of AMA DEUS are based on piezo-ceramics elements for the broadband recording of s ignals with frequencies ranging up to 125kHz.\nAcoustic data are continuou sly acquired and processed by applying online filter algorithms to pre-sel ect a high-purity sample of neutrino-like signals. Transient signals in th e deep sea are of manifold origin and can mimic the acoustic signature of a neutrino interaction. In order to assess the background for acoustic neu trino detection in the deep sea\, the characteristics of these transient s ignals and of the ambient noise have been investigated. To this end\, an o ffline analysis package for the pre-selected data was developed\, includin g signal classification and acoustic source reconstruction algorithms. To test and validate the performance of the analysis package and to simulate the response of the system to neutrino interactions\, a complete simulati on chain was developed.\nIn the presentation\, the AMADEUS system will be described. Selected recent AMADEUS results will be discussed and first con clusions concerning the feasibility of acoustic detection of ultra-high-en ergy neutrinos in the Mediterranean Sea presented.\n\nhttps://events.icec ube.wisc.edu/event/55/contributions/3927/ URL:https://events.icecube.wisc.edu/event/55/contributions/3927/ END:VEVENT BEGIN:VEVENT SUMMARY:Modeling radio emission from particle showers in dense media and a ir: a pedagogical overview. DTSTART:20140609T181000Z DTEND:20140609T185000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3928@events.icecube.wisc.edu DESCRIPTION:Speakers: Alvarez-Muniz Jaime (Dept\, of Particle Physics\, Un iv. of Santiago de Compostela\, Spain)\n\nI will review the current unders tanding of radio emission from particle\nshowers in both dense dielectric media and the atmosphere. A net charge\nis generated in those showers due to the Askaryan effect in dense media\,\nand to Askaryan as well as geomag netic effects in air. I will discuss macroscopic\nand microscopic approach es to model the emitted radiation. The prominent role\nof shock wave effec ts similar to those observed in Cherenkov radiation will\nbe emphasized.\n \nhttps://events.icecube.wisc.edu/event/55/contributions/3928/ URL:https://events.icecube.wisc.edu/event/55/contributions/3928/ END:VEVENT BEGIN:VEVENT SUMMARY:ANITA: analysis and program status DTSTART:20140612T140000Z DTEND:20140612T142000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3929@events.icecube.wisc.edu DESCRIPTION:Speakers: David Seckel (University of Delaware)\n\nA review of the instrument and science program is given\, including the status of rea nalysis of the cosmic ray events detected by the ANITA-I payload\, and pla ns for ANITA-III.\n\nhttps://events.icecube.wisc.edu/event/55/contribution s/3929/ URL:https://events.icecube.wisc.edu/event/55/contributions/3929/ END:VEVENT BEGIN:VEVENT SUMMARY:The effects of surface roughness on lunar Askaryan pulses DTSTART:20140611T203500Z DTEND:20140611T205500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3930@events.icecube.wisc.edu DESCRIPTION:Speakers: Clancy James (University of Erlangen-Nuernberg)\n\nT he effects of lunar surface roughness\, on both small and large scales\, o n Askaryan radio pulses generated by particle cascades beneath the lunar s urface has never been fully estimated. Surface roughness affects the chanc es of a pulse escaping the lunar surface\, its coherency\, and the charact eristic detection geometry. It will affect the expected signal shape\, the relative utility of different frequency bands\, the telescope pointing po sitions on the lunar disk\, and most fundamentally\, the chances of detect ing the known UHE cosmic ray and any prospective UHE neutrino flux. Near-f uture radio-telescopes such as FAST and the SKA promise to be able to dete ct the flux of cosmic rays\, and it is critical that surface roughness be treated appropriately in simulations. of the lunar Askaryan technique.\nIn this contribution\, a facet model for lunar surface roughness is combined with a method to propagate coherent radio pulses through boundaries to es timate the full effects of lunar surface roughness on neutrino-detection p robabilities. The method is able to produce pulses from parameterised part icle cascades beneath the lunar surface as would be viewed by an observer at Earth\, including all polarisation and coherency effects. Results from this calculation are presented for both characteristic cosmic ray and neut rino cascades\, and estimates of the effects mentioned above - particular ly signal shape\, frequency-dependence\, and sensitivity - are presented.\ n\nhttps://events.icecube.wisc.edu/event/55/contributions/3930/ URL:https://events.icecube.wisc.edu/event/55/contributions/3930/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio detection of Cosmic Rays in the GHz band at the Pierre Auger Observatory DTSTART:20140610T161000Z DTEND:20140610T164000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3931@events.icecube.wisc.edu DESCRIPTION:Speakers: Imen Al Samarai (IPNO)\n\nObservations of microwave radiation emitted by low energy electrons left after the passage of a high energy electron beam in accelerator experiments offered new possibilities of Ultra High Energy Cosmic Rays (UHECR) detection techniques based on mi crowave radiation. This would bring a tenfold increase in detector duty cy cle compared to the standard fluorescence technique.\nThe emission mechani sm interpreted as Molecular Bremsstrahlung Radiation (MBR) is expected to produce an unpolarized and isotropic signal. Motivated by the expected ful l duty cycle of such a technique and to its insensitivity to atmospheric a ttenuation\, three microwave detectors\; EASIER\, MIDAS and AMBER are impl emented in Auger.\nThe status and results of these microwave detectors are reported.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3931/ URL:https://events.icecube.wisc.edu/event/55/contributions/3931/ END:VEVENT BEGIN:VEVENT SUMMARY:An estimate of the spectral intensity expected from the molecular Bremsstrahlung radiation in extensive air showers DTSTART:20140611T182500Z DTEND:20140611T184500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3932@events.icecube.wisc.edu DESCRIPTION:Speakers: Romain Gaior (LPNHE)\, Ioana Maris (UGR)\, Miguel Bl anco (LPNHE)\, Mariangela Settimo (LPNHE)\, Julien Aublin (LPNHE)\, Pierre Billoir (LPNHE)\, Antoine Letessier-Selvon (LPNHE)\, Francesco Salamida ( IPNO)\, Patrick Stassi (LPSC)\, Anne Stutz (LPSC)\, Sandra Le Coz (LPSC)\, François Montanet (LPSC)\, Didier Lebrun (LPSC)\, Corinne Berat (LPSC)\, Isabelle Lhenry-Yvon (IPNO)\, Olivier Deligny (CNRS/IN2P3 - IPN Orsay)\, Imen Al Samarai (IPNO)\n\nA detection technique of Ultra High Energy Cosm ic Rays (UHECR) complementary to fluorescence and Radio techniques would b e the use of the Molecular Bremsstrahlung Radiation (MBR) emitted by low e nergy electrons left after the passage of the showers in the atmosphere.\n \nThe emission mechanism is expected from quasi-elastic collisions of elec trons produced in the shower by the ionization of molecules in the atmosph ere.\n\nIn this contribution\, we calculate the spectral intensity of phot ons at ground level originating from the transition bet ween unquantize d energy states of free ionization electrons.\n\nIn the absence of absorpt ion of the emitted photons in the plasma\, we obtain a spectral intensity depending on the effective lifetime of the ionization electrons and compar e it to the spectral intensity measurements provided by the SLAC experimen t (Gorham et al. 2008).\n\nhttps://events.icecube.wisc.edu/event/55/contri butions/3932/ URL:https://events.icecube.wisc.edu/event/55/contributions/3932/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigating the extensive air shower properties using the polari zation and frequency features of the radio signals measured by the CODALEM A autonomous station array. DTSTART:20140610T131000Z DTEND:20140610T134000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3933@events.icecube.wisc.edu DESCRIPTION:Speakers: Lilian Martin (SUBATECH)\, Collaboration CODALEMA (S UBATECH/LESIA/USN)\n\nCODALEMA is the last experiment currently running in Europe dedicated to the extensive air shower detection using the observat ion of its induced radio electric field and with the ambition to promote t his radio detection technique to a mature technology suited to a next gene ration giant cosmic ray observatory. The latest experimental upgrade of CO DALEMA consisting in a large array of autonomous stations will be presente d with a special emphasis put on the key technical features of this instru ment. While the relative timings and the amplitudes of the electric field measured by antennas are now widely used to characterize the extensive air showers\, the polarization patterns and the frequency contents are consid ered now as very useful information to strongly improve these measurement capabilities. The latest results obtained by the dual-polarization wide-ba nd antennas of CODALEMA will be reviewed and their impact in terms of inst rumental design and optimization will be investigated.\n\nhttps://events.i cecube.wisc.edu/event/55/contributions/3933/ URL:https://events.icecube.wisc.edu/event/55/contributions/3933/ END:VEVENT BEGIN:VEVENT SUMMARY:Geant4 simulations of radio signals from particle showers for the SLAC T-510 experiment DTSTART:20140609T191500Z DTEND:20140609T193500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3934@events.icecube.wisc.edu DESCRIPTION:Speakers: Anne Zilles (KIT)\, SLAC T-510 Collaboration (SLAC)\ n\nThe SLAC T-510 experiment was designed to reproduce the physics of radi o emission from air showers in a controlled lab experiment with the goal t o test established formalisms for simulation of radio emission physics: th e “end-point" formalism and the "ZHS" formalism.\nSimulation results der ived with these formalisms can be explained by a superposition of magnetic ally induced transverse current radiation and the Askaryan (charge-excess) effect.\nHere\, we present results of Geant4 simulations of the experimen t with both formalisms\, taking into account the details of the experiment al setup (beam energy\, target geometry and material\, magnetic field conf iguration and refraction effects) to test this hypothesis.\n\nhttps://even ts.icecube.wisc.edu/event/55/contributions/3934/ URL:https://events.icecube.wisc.edu/event/55/contributions/3934/ END:VEVENT BEGIN:VEVENT SUMMARY:LOPES-3D – studies on the benefits of direct measurements with v ertically aligned antennas DTSTART:20140611T155000Z DTEND:20140611T161000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3935@events.icecube.wisc.edu DESCRIPTION:Speakers: Daniel Huber (KIT)\, Tim Huege (Karlsruhe Institute of Technology)\n\nThe LOPES experiment was a radio interferometer built at the existing air shower array\nKASCADE-Grande in Karlsruhe\, Germany. The last configuration of LOPES was called LOPES-3D and\nconsisted of ten tri pole antennas. Each of these antennas consisted of three crossed dipoles e ast-west\, north-south\nand vertically aligned. With this\, LOPES-3D had t he unique possibility to study the benefits of additional\, direct\nmeasur ements with vertically aligned antennas in the environment of the well und erstood and calibrated particle\ndetector array KASCADE-Grande. The measur ements with three spacial coincident antennas led to a redundant\nreconstr uction of the E-field vector. Thus\, several methods to exploit the redund ancy were developed and tested.\nFurthermore\, for the first time\, the ba ckground noise could be studied polarization- and direction dependent.\nWi th LOPES-3D it could be demonstrated that radio detection reaches a higher efficiency for inclined showers\nand that the vertical component gets mor e important for the measurement of inclined showers.\nIn this contribution we discuss the development of different weighting schemes for the best co mbination of the\nthree redundant reconstructed E-field vectors. Furthermo re we discuss the influence of these weighting schemes\non the ability to reconstruct the showers in radio and on the geometry reconstruction. We sh ow an estimate of the\nradio efficiency for inclined showers with focus on the benefits of measurements with vertically aligned\nantennas and we pre sent the direction dependent noise in the different polarizations.\n\nhttp s://events.icecube.wisc.edu/event/55/contributions/3935/ URL:https://events.icecube.wisc.edu/event/55/contributions/3935/ END:VEVENT BEGIN:VEVENT SUMMARY:A dedicated antenna array for radio detection of Extended Air Show ers. DTSTART:20140611T151000Z DTEND:20140611T153000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3936@events.icecube.wisc.edu DESCRIPTION:Speakers: Alain Lecacheux (CNRS - Observatoire de Paris)\, Lil ian MARTIN (SUBATECH-UMR6457)\, Didier CHARRIER (SUBATECH-UMR6457)\, Richa rd Dallier (SUBATECH-UMR6457)\, Laurent DENIS (Nançay Radio astronomy Sta tion)\n\nRadio pulses associated with Extended Air Showers (EAS) produced in terrestrial atmosphere by High Energy Cosmic Rays (UHECR) of energy 10^ 17 eV and above\, are now routinely observed by dedicated radio instrument s on ground. This may offer a new and appealing way for elucidating the na ture and origin of involved primary particles\, an open question still uns olved. \nUnfortunately\, the high occupancy of the electromagnetic spectru m by undesired signals from natural and anthropogenic origins has made una mbiguous EAS radio detection a challenging problem. Former attempts based on timing coincidences from several independent radio antennas\, or using auxiliary triggering by conventional particle detectors\, are still not fu lly satisfying.\nWe present here a solution based on real time\, coherent radio detection by using a small array of 10x2 cross polarized dipoles\, d istributed over a 150m x 150m surface area and operated in continuous sky surveying mode. \nPreliminary results obtained with the new system are b riefly reviewed and discussed.\nThe final detection scheme will be achieve d by using on line\, fast computing software based on a dedicated unsuperv ised recognition algorithm. \nThe new array is a part of the CODALEMA expe riment located in Nançay radio astronomy observatory (France).\n\nhttps:/ /events.icecube.wisc.edu/event/55/contributions/3936/ URL:https://events.icecube.wisc.edu/event/55/contributions/3936/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the cosmic ray mass composition with the LOFAR radi o telescope DTSTART:20140611T132000Z DTEND:20140611T134000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3937@events.icecube.wisc.edu DESCRIPTION:Speakers: Stijn Buitink (Radboud University Nijmegen\, Netherl ands)\n\nLOFAR is a multipurpose radio telescope which can be used for rad io detection of cosmic rays while running astronomical observations at the same time. In the dense core individual air showers are detected by hundr eds of dipole antennas. The raw electromagnetic waveform as detected by ea ch antenna is stored in a five-second ring buffer\, which is read out when a trigger is issued by the LORA particle detector array. Hundreds of show ers with energies above 10$^17$ eV have been measured in two frequency reg imes: low band (10-90 MHz) and high band (110-250 MHz).\n\nThe complicated radio emission pattern on the ground can be accurately reproduced by mode rn radio simulation codes and contains information about the longitudinal shower development. With a hybrid reconstruction technique\, we can measur e the depth of the shower maximum with an accuracy of ~20 g/cm^2 in the en ergy regime of 10^17 eV to 10^18 eV. Cosmic-ray mass measurements in this range are of particular interest as it may harbor the transition from a Ga lactic to an extragalactic origin. We present a mass composition analysis based on the first results and discuss their implications for transition m odels.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3937/ URL:https://events.icecube.wisc.edu/event/55/contributions/3937/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio detection of neutrinos DTSTART:20140609T135000Z DTEND:20140609T142000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3938@events.icecube.wisc.edu DESCRIPTION:Speakers: Kara Hoffman (o=umd\,ou=Institutions\,dc=icecube\,dc =wisc\,dc=edu)\n\nTBD\n\nhttps://events.icecube.wisc.edu/event/55/contribu tions/3938/ URL:https://events.icecube.wisc.edu/event/55/contributions/3938/ END:VEVENT BEGIN:VEVENT SUMMARY:From the earth to the moon. DTSTART:20140611T195500Z DTEND:20140611T203500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3939@events.icecube.wisc.edu DESCRIPTION:Speakers: Olaf Scholten (KVI-CART\, Univ. of Groningen)\n\nTBD \n\nhttps://events.icecube.wisc.edu/event/55/contributions/3939/ URL:https://events.icecube.wisc.edu/event/55/contributions/3939/ END:VEVENT BEGIN:VEVENT SUMMARY:Lake Baikal acoustic neutrino activities DTSTART:20140609T145000Z DTEND:20140609T151500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3940@events.icecube.wisc.edu DESCRIPTION:Speakers: Nikolay Budnev (Irkutsk State University)\n\nTBD\n\n https://events.icecube.wisc.edu/event/55/contributions/3940/ URL:https://events.icecube.wisc.edu/event/55/contributions/3940/ END:VEVENT BEGIN:VEVENT SUMMARY:Muppets and the EeV sky DTSTART:20140609T131000Z DTEND:20140609T135000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3941@events.icecube.wisc.edu DESCRIPTION:Speakers: Francis Halzen (University of Wisconsin-Madison)\n\n TBD\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3941/ URL:https://events.icecube.wisc.edu/event/55/contributions/3941/ END:VEVENT BEGIN:VEVENT SUMMARY:Ice surface roughness modeling for effect on radio signals from UH E particle showers DTSTART:20140609T213000Z DTEND:20140609T215000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3942@events.icecube.wisc.edu DESCRIPTION:Speakers: Jessica Stockham (University of Kansas)\n\nFor radio antenna neutrino and cosmic ray detectors located in or above the Antarct ic ice sheet\, the reconstruction of both ultra-high energy (UHE) neutrino and cosmic ray air shower events requires knowledge the transmission and reflection properties of the air-ice interface. To better understand these properties\, in-lab and field data will be obtained and analyzed. The in- lab experiment will measure reflected power from rough surfaces of a granu lar material in the frequency range of 2-3GHz. These meausrements are used to determine a model capable of predicting reflected power as a function of elevation angle and frequency based on measurable parameters of the sur face and material. Field data is taken in the form of stereoscopic images of the surface as part of the Antarctic Geophysics Along the Vostok Expedi tion (AGAVE). 3D data from the stereoscopic images will be used to create similarly rough and appropriately scaled surfaces in the lab for compariso n to the results of the reflection model and to the models currently being used for simulation and reconstruction of shower events.\n\nhttps://event s.icecube.wisc.edu/event/55/contributions/3942/ URL:https://events.icecube.wisc.edu/event/55/contributions/3942/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of the polarization of the radio emission in air showe rs with LOFAR and the influence of atmospheric electric fields. DTSTART:20140609T193500Z DTEND:20140609T195500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3943@events.icecube.wisc.edu DESCRIPTION:Speakers: Olaf Scholten (KVI-CART\, Univ. of Groningen)\, Stij n Buitink (Radboud University Nijmegen\, Netherlands)\, Anna Nelles (Radbo ud University Nijmegen)\n\nWith the LOFAR antenna array we have measured t he the polarization footprint of the radio emission from extensive air sho wers for a large number of single events. The polarization direction is de termined from the Stokes parameters integrated over the time duration of t he radio pulse.\nIt will be shown that for events for which no thunderstor m activity has been registered the polarization pattern obeys very well th e expected characteristics based on a superposition of a geomagnetically-i nduced transverse current and charge excess contributions. The core-distan ce dependence of ratio of the two contributions is measured.\nFor events w here thunderstorm activity is registered strong deviations from the fair-w eather polarization pattern are observed. A semi-quantitative interpretati on of the influence of atmospheric electric fields on the polarization pat tern will be presented.\n\nhttps://events.icecube.wisc.edu/event/55/contri butions/3943/ URL:https://events.icecube.wisc.edu/event/55/contributions/3943/ END:VEVENT BEGIN:VEVENT SUMMARY:End to end calibration of the ARA detector DTSTART:20140612T155000Z DTEND:20140612T161000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3944@events.icecube.wisc.edu DESCRIPTION:Speakers: Keiichi Mase (Chiba University)\n\nCoherent Cherenko v radio emissions from particle cascades were predicted by Askaryan\, and the emissions were firstly detected at SLAC from the electro-magnetic casc ades. Askaryan Radio Array (ARA) is being built at the South Pole to obser ve cosmogenic neutrinos by detecting the coherent radio emissions with the large instrumental area of about 100 km^2. We are planning an end to end calibration of the ARA detectors by using a LINAC installed at the Telesco pe Array experiment site. The detail of the calibration and the current st atus will be presented.\n\nhttps://events.icecube.wisc.edu/event/55/contri butions/3944/ URL:https://events.icecube.wisc.edu/event/55/contributions/3944/ END:VEVENT BEGIN:VEVENT SUMMARY:First data analysis steps for the Askaryan Radio Array stations DTSTART:20140612T153000Z DTEND:20140612T155000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3945@events.icecube.wisc.edu DESCRIPTION:Speakers: Thomas Meures (o=ulb\,ou=Institutions\,dc=icecube\,d c=wisc\,dc=edu)\n\nThe Askaryan Radio Array (ARA) is one of the future neu trino observatories focusing on the detection of GZK-neutrinos with energi es beyond 1017eV through secondary radio waves. Observing GZK-neutrinos is especially interesting because it is one of the few ways to investigate t he CR-spectrum beyond the observed GZK-cutoff. These neutrinos\, when reac hing the earth\, produce particle cascades in different media like ice and rock salt which\, in case of the above mentioned energies\, emit detectab le radio waves through the Askaryan effect.\nARA is currently in the build ing phase and will be optimized to detect the radio emission from neutrino induced cascades with primary energies greater than 1017eV. A grid of 37 antenna clusters\, spaced by 2 km\, is planned to be deployed in the South Pole ice\, at a depth of 200 m. The full ARA detector will cover an instr umented area of about 100 km2\, and as built will be the most cost-effecti ve neutrino detector in the energy range between 1017eV and 1019eV.\nThree ARA stations\, each consisting of 16 measurement antennas\, and one proto type station are already deployed in the ice. All of them are functioning as independent detectors each with full detection and reconstruction capab ilities.\nIn this contribution\, the first analysis steps of data from two of the three stations are presented.\n\nhttps://events.icecube.wisc.edu/e vent/55/contributions/3945/ URL:https://events.icecube.wisc.edu/event/55/contributions/3945/ END:VEVENT BEGIN:VEVENT SUMMARY:Advanced Reconstruction Strategies for the Auger Engineering Radio Array DTSTART:20140611T134000Z DTEND:20140611T140000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3946@events.icecube.wisc.edu DESCRIPTION:Speakers: Qader Dorosti Hasankiadeh (Karlsruher Institut für Technologie (KIT)\;)\n\nThe Auger Engineering Radio Array (AERA) aims to d etect extensive air showers caused by the interactions of ultra-high energ y cosmic rays with the Earth atmosphere\, providing complementary informat ion to the Auger surface\, fluorescence and muon detectors. The second st age of AERA\, currently consisting of 124 radio stations\, has been comple ted at the Pierre Auger Observatory in early 2013\, comprising a larger d etection area compared to the first stage of AERA (AERA-24).\nThe main obj ective for exploiting a radio detector is to precisely measure the fundame ntal air-shower parameters\, such as the direction\, energy and compositio n. To this end\, we have developed reconstruction strategies and algorithm s to measure the air-shower parameters with high efficiency. \n We will di scuss the reconstruction strategies developed to determine the fundamental air-shower parameters. In addition\, we will present the results obtained by applying the reconstruction strategies on a fraction of the experiment al data.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3946/ URL:https://events.icecube.wisc.edu/event/55/contributions/3946/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent developments in the construction of a line array projector for the calibration of Acoustic Neutrino Telescopes DTSTART:20140609T160000Z DTEND:20140609T162000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3947@events.icecube.wisc.edu DESCRIPTION:Speakers: Sean Danaher (Northumbria University)\n\nRecent deve lopments in the construction of a line array projector for the calibration of Acoustic Neutrino Telescopes\n\nhttps://events.icecube.wisc.edu/event/ 55/contributions/3947/ URL:https://events.icecube.wisc.edu/event/55/contributions/3947/ END:VEVENT BEGIN:VEVENT SUMMARY:An autonomous method for drilling deep in South Pole ice DTSTART:20140612T163000Z DTEND:20140612T165000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3948@events.icecube.wisc.edu DESCRIPTION:Speakers: Rolf Nahnhauer (DESY)\n\nInformation about thermal p robes and how to use them for autonomous deep drilling in ice will be give n. The method presented may be useful for drilling holes at large distance s and/or large numbers\, necessary for building big (hybrid) arrays for co smogenic neutrino detection.\n\nhttps://events.icecube.wisc.edu/event/55/c ontributions/3948/ URL:https://events.icecube.wisc.edu/event/55/contributions/3948/ END:VEVENT BEGIN:VEVENT SUMMARY:Measuring and parameterizing the two-dimensional pattern of radio emission in air showers with LOFAR DTSTART:20140611T130000Z DTEND:20140611T132000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3949@events.icecube.wisc.edu DESCRIPTION:Speakers: Anna Nelles (Radboud University Nijmegen)\, Collabor ation LOFAR (ASTRON\, The Netherlands)\n\nThe detection of radio emission of air showers has rapidly advanced in the past years. New experiments hav e shed light on the details of the emission and air shower simulations pro vide rather accurate models of the measured emission. To exploit radio emi ssion in large-scale experiments\, a simple and analytic parametrization o f the distribution of the radio signal at ground level is needed. Such a p arametrization can allow for fast calculations of the expected signals and can be used to reconstruct the geometry of the measured air showers. Data taken with the Low- Frequency Array (LOFAR) show a complex two-dimensiona l pattern of pulse powers\, which is sampled with hundreds of antennas per event. Earlier parametrizations of the lateral signal distribution have p roven insufficient to describe these highly detailed data.\n\nWe present a two-dimensional model with five free parameters derived from air-shower s imulations. All parameters show strong correlations with air shower prope rties\, such as the energy of the shower\, the arrival direction\, and the height of the shower maximum. This parametrization represents the data ta ken with LOFAR very accurately. We present the application of this method to LOFAR data and discuss implications for the reconstruction of the showe r geometry.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3949 / URL:https://events.icecube.wisc.edu/event/55/contributions/3949/ END:VEVENT BEGIN:VEVENT SUMMARY:Tunka-Rex experiment for detection of air-shower radio emission DTSTART:20140610T151000Z DTEND:20140610T154000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3950@events.icecube.wisc.edu DESCRIPTION:Speakers: Yuliya Kazarina (Physical faculty\, Irkutsk State Un iversity\, Irkutsk\, Russian Federation)\, Collaboration Tunka-Rex (KIT\, API ISU\, SINP MSU\, INR RAS\, DEZY)\n\nThe Tunka-Rex experiment (Tunka Ra dio Extension) was created in 2012 at the Tunka Valley (Republic of Buryat ia\, Russia). Its purpose is to investigate methods for the energy spectru m and the mass composition of high energy cosmic rays based on the radio e mission of air showers. Tunka-Rex is an array of 25 radio antennas distrib uted over an area of 3 km2. The most important feature of the project is t hat the air-shower radio emission is measured in coincidence with the Tunk a-133 installation\, which detects the Cherenkov radiation generated by th e same atmospheric showers. Joint measurements of the radio emission and t he Cherenkov light provide a unique opportunity for crosscalibration of bo th calorimetric detection methods. The main goal of Tunka-Rex is to determ ine the precision for the reconstruction of air-shower parameters using th e radio detection technique. This report presents the current status of Tu nka-Rex\, and first results of Tunka-Rex including a discussion of the rec onstruction methods for the parameters of the primary cosmic rays.\n\nhttp s://events.icecube.wisc.edu/event/55/contributions/3950/ URL:https://events.icecube.wisc.edu/event/55/contributions/3950/ END:VEVENT BEGIN:VEVENT SUMMARY:Technological developments for the Auger Engineering Radio Array ( AERA) DTSTART:20140611T145000Z DTEND:20140611T151000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3951@events.icecube.wisc.edu DESCRIPTION:Speakers: Jennifer Maller (Subatech)\, The Pierre Auger Collab oration (.)\n\nThe Auger Engineering Radio Array consists of 124 radio sta tions covering 6 km² installed within the low energy extension of the Pie rre Auger Observatory in Argentina\; this location allows a multi-hybrid m easurement of air-showers with the fluorescence telescopes\, the water-Che renkov and the muon detectors close to the radio array. AERA detects the r adio emission from cosmic-ray induced air showers above 10^17 eV. The meas ured electric field is used to constrain the characteristics of the primar y particle: arrival direction\, energy and particle type (mass). These stu dies are possible due to an instrumentation development allowing externall y-triggered in parallel with self-triggered measurements in the MHz domain and an improved understanding of the radio emission processes.\nWe will p resent the main technological developments of AERA that have been realized since 2010\, within the Pierre Auger collaboration\, to reach the request ed quality allowing the accurate measurement of the electric field emitted by air showers. We will review the antennas and their Low Noise Amplifier s\, the trigger board and the full acquisition chain up to the communicati on system. The current R&D on new technical developments will be also disc ussed.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3951/ URL:https://events.icecube.wisc.edu/event/55/contributions/3951/ END:VEVENT BEGIN:VEVENT SUMMARY:Simulation chain and signal classification for acoustic neutrino d etection in sea water DTSTART:20140609T154000Z DTEND:20140609T160000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3952@events.icecube.wisc.edu DESCRIPTION:Speakers: Dominik Kiessling (Erlangen Centre for Astroparticle Physics)\n\nAcoustic neutrino detection is a promising approach to extend the energy range of neutrino telescopes to energies beyond 10^{18} eV. Cu rrent water-Cherenkov-neutrino-telescopes\, like e.g. KM3NeT\, include aco ustical sensors in addition to the optical ones. While the main purpose of these acoustic sensors is the position calibration of the detection units \, they could be used as instruments for acoustic detection\, too. In this article a Monte Carlo simulation chain for acoustic detectors will be pre sented\, covering the initial interaction of the neutrino up to the signal classification of recorded events. The ambient and transient background i n the simulation were implemented according to the data recorded by the ac oustic set-up AMADEUS in ANTARES. The effects of refraction on the neutrin o signature in the detector are studied\, and a classification of the reco rded events is implemented. As bipolar waveforms similar to those of the e xpected neutrino signals are also emitted from other sound sources\, addit ional features like the geometrical shape of the propagation have to be co nsidered for the signal classification. This leads to a large improvement of the background suppression by almost two orders of magnitude\, since th e cylindrical "pancake" propagation pattern is a distinctive trait of neut rino signals. An overview of the simulation chain and the signal classific ation will be presented and preliminary studies of the performance of the classification will be discussed.\n\nhttps://events.icecube.wisc.edu/event /55/contributions/3952/ URL:https://events.icecube.wisc.edu/event/55/contributions/3952/ END:VEVENT BEGIN:VEVENT SUMMARY:Wavefront of the Radio Emission from Air Showers DTSTART:20140609T205000Z DTEND:20140609T211000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3953@events.icecube.wisc.edu DESCRIPTION:Speakers: Frank Schröder (Karlsruhe Institute of Technology ( KIT))\, Collaboration LOPES (-)\n\nWe investigated the radio wavefront of cosmic-ray air showers with LOPES measurements and CoREAS simulations: the wavefront is of hyperbolic shape and can be used to reconstruct the showe r maximum.\n\nLOPES was a digital\, interferometric antenna array at the K arlsruhe Institute of Technology (KIT) at an altitude of 110 m. LOPES cons isted of up to 30 antennas on an area with approximately 200 m diameter. I t was externally triggered by the KASCADE particle detector array and meas ured the radio emission of air showers in the effective band from 43 to 74 MHz. Our analysis is based on 316 LOPES events with energies above 0.1 Ee V and zenith angles below 45°. In addition\, we have made two CoREAS simu lations of the radio wavefront for each event\, one for a proton and one f or an iron nucleus as primary particle.\n\nA hyperbola describes the wavef ront shape significantly better than a sphere or a cone. On the one hand\, this means that the radio emission cannot be approximated by a static poi nt source at the shower maximum. On the other hand\, a conical wavefront e xpected for a moving point source seems to be a sufficient approximation f or axis distances > 50 m.\n\nIn first order\, the angle between the shower plane and the limiting cone of the hyperbola depends on the distance of t he radio array to the shower maximum. This implies dependences on the zeni th angle as well as on the atmospheric depth of the shower maximum\, Xmax. We exploit this for the reconstruction of Xmax based on the arrival times of the signal in the individual antennas. For the simulations\, we obtain a resolution of approximately 25 g/cm². For the measurements\, the resol ution is only 140 g/cm²\, since LOPES in its radio-loud environment suffe rs from significant experimental uncertainties.\n\nhttps://events.icecube. wisc.edu/event/55/contributions/3953/ URL:https://events.icecube.wisc.edu/event/55/contributions/3953/ END:VEVENT BEGIN:VEVENT SUMMARY:Use of Radar Depth Sounding Data to Estimate Radio Frequency Atten uation in Greenlandic and Antarctic Ice DTSTART:20140612T161000Z DTEND:20140612T163000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3954@events.icecube.wisc.edu DESCRIPTION:Speakers: Mark Stockham (University of Kansas)\n\nAntarctic ic e represents the interaction volume for multiple UHE neutrino experiments. When neutrinos collide with ice particles they produce radio waves that p ropagate to in-ice\, surface\, or balloon-borne detectors. The radio frequ ency signal strength observed at the detector\, however\, depends on the r adio frequency attenuation length of the ice through which the neutrino-ge nerated signal must travel. Attenuation length is a location-specific ice property and varies mainly as a function of temperature and chemistry. The Center for Remote Sensing of Ice Sheets (CReSIS) project has data from ma ny locations in Antarctica and Greenland produced by radar depth sounding. Using methods developed by analyzing the continuum signal in radar depth sounding data from Greenland depth-dependent attenuation length estimates are compared to estimates derived from ice core data. Comparisons between Greenlandic and colder Antarctic ice will also be made.\n\nhttps://events. icecube.wisc.edu/event/55/contributions/3954/ URL:https://events.icecube.wisc.edu/event/55/contributions/3954/ END:VEVENT BEGIN:VEVENT SUMMARY:PRIDE – Passive Radio Ice Depth Experiment - An Instrument to Me asure Outer Planet Lunar Ice Depths from Orbit using EHE Neutrinos DTSTART:20140611T205500Z DTEND:20140611T211500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3955@events.icecube.wisc.edu DESCRIPTION:Speakers: Amy Connolly (Ohio State University)\, Andrew Romero -Wolf (JPL)\, Stuart Kleinfelder (UCI)\, David Besson (KU)\, Steven Barwic k (UCI)\, Grant Stephens (Johns Hopkins University Applied Physics Laborat ory)\, Brian Sequeira (Johns Hopkins University Applied Physics Laboratory )\, Gerald Patterson (Johns Hopkins University Applied Physics Laboratory) \, Robert Schaefer (Johns Hopkins University Applied Physics Laboratory)\, Timothy Miller (Johns Hopkins University Applied Physics Lab)\n\nWe descr ibe a potential confluence between EeV neutrino detection and planetary sc ience: a concept for an instrument to measure the thickness of the ice sh ell on a planetary body\, such as Jupiter’s moon Europa or Saturn’s mo on Enceladus\, by making use of the Askaryan Effect RF signal from EHE neu trinos observed from an orbiting spacecraft. Unlike a large high powered a ctive device\, i.e.\, an ice-penetrating radar\, this instrument is a pass ive receiver of the naturally occurring signal generated by interactions o f deep penetrating cosmic ray neutrinos in the extremely thick\, cold ice layer encasing outer solar system moons. It is therefore potentially less massive and requires less power\, making it very attractive for interplan etary missions. Measuring the ice sheet thickness on such moons is a first step toward exploring potential oceans below\, and is a very high scienti fic priority for outer planet missions\, so new and economical approaches to this measurement are of great interest. We discuss the basic concept\, including the correlations of event rate and direction distribution with ice sheet thickness\, and consider the instrument design requirements from the perspective of a NASA Outer Planet Orbiter Mission. We show results [ 1] of simulations\, compare signal-to-noise estimates\, and examine possib le components and configurations for the antenna\, receiver\, and electron ics. We note some options that can be used to reduce mass and power. Final ly\, we identify issues that would need further study to produce a more co ncrete design. \n[1] Miller\, T.\, Schaefer\, R.K.\, and Sequeira\, H.B.\, Icarus\, 220\, 877-888\, 2012.\n\nhttps://events.icecube.wisc.edu/event/5 5/contributions/3955/ URL:https://events.icecube.wisc.edu/event/55/contributions/3955/ END:VEVENT BEGIN:VEVENT SUMMARY:Precision measurements of the shower front of the radio emission i n air showers with LOFAR DTSTART:20140610T134000Z DTEND:20140610T141000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3956@events.icecube.wisc.edu DESCRIPTION:Speakers: Joerg Hoerandel (Radboud University Nijmegen)\n\nHig h-energy cosmic rays impinging onto the atmosphere of the Earth initiate c ascades of secondary particles: extensive air showers. The electrons and p ositrons in air showers interact with the geomagnetic field and emit radia tion\, which we record in the tens-of-MHz regime. The LOFAR radio telescop e measures the radio emission with high antenna density and two polarizati on directions. We used LOFAR for measurements of the shape of the radio wa ve front of air showers with unprecedented precision with sub-nanosecond r esolution. Our measurements show that the radio shower front is described best by a hyperboloid - it fits the data significantly better than the sha pes discussed in the literature (conical and spherical shapes). We present recent results and show a quantitative comparison of different shapes ana lyzed. These results put strong constraints on the models to describe the radio emission in air showers. We also point out correlations between the shape of the shower front and the properties of the shower-inducing primar y particle.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3956 / URL:https://events.icecube.wisc.edu/event/55/contributions/3956/ END:VEVENT BEGIN:VEVENT SUMMARY:Performance of the ARIANNA Neutrino Telescope DTSTART:20140612T133000Z DTEND:20140612T140000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3957@events.icecube.wisc.edu DESCRIPTION:Speakers: Corey Reed (UC Irvine)\n\nThe ARIANNA experiment use s low noise\, low power and inexpensive\ntechnology to search for radio pu lses emitted by extremely high energy\ncosmic neutrino interactions. Three detector stations have been\ndeployed in the Ross Ice Shelf of Antarctica \, taking both\nenvironmental as well as radio pulse data. The stations ar e powered by\nsolar and wind generators and transfer data north via wirele ss\nInternet and satellite modem peripherals. The performance of the\nstat ions in 2014 will be discussed and the effectiveness of the Ross\nIce Shel f as a radio quiet environment will be examined. Preliminary\nsearches for neutrino signals in the data will be presented.\n\nhttps://events.icecube .wisc.edu/event/55/contributions/3957/ URL:https://events.icecube.wisc.edu/event/55/contributions/3957/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing a two component approach to describe radio emission from a ir showers DTSTART:20140609T203000Z DTEND:20140609T205000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3958@events.icecube.wisc.edu DESCRIPTION:Speakers: Jaime Alvarez-Muniz (Univ. Santiago de Compostela\, Spain)\, Washington R. Carvalho Jr. (Univ. Santiago de Compostela\, Spain) \, Harm Schoorlemmer (Univ. of Hawaii)\, Enrique Zas (Univ. of Santiago de Compostela\, Spain)\n\nThe radiation emitted by atmospheric showers is cu rrently interpreted in terms of the deviation of the charged particles in the magnetic field of the Earth and the emission due to the charge excess (Askary'an effect). Each of these mechanisms has a distinctive polarizatio n. The complex signal patterns obtained both in dedicated experiments meas uring average behaviors and in simulations\, can be qualitatively explaine d as the interference (superposition) of the fields induced by each mechan ism.\n\nThis work is an attempt to explicitly and quantitatively test a si mple phenomenological model based on this idea (two dominant emission mech anisms). The model is constructed by isolating each of the two components at the simulation level and by making use of \napproximate symmetries for each of the contributions separately. The results of the model are then ch ecked against full ZHAireS simulations of the electric field calculated fr om first principles. With these simulations\, that are now known to reprod uce experimental data\, we show that the simple model describes radio emis sion at a few percent level in a wide range of shower-observer geometries and on a shower-by-shower basis. This conclusion converts this approach in a simple method to reduce the computing time needed to accurately predict the electric field of radio pulses emitted from air showers\, with many p ractical applications \nin experimental situations of interest.\n\nhttps:/ /events.icecube.wisc.edu/event/55/contributions/3958/ URL:https://events.icecube.wisc.edu/event/55/contributions/3958/ END:VEVENT BEGIN:VEVENT SUMMARY:Detection of Radio Emission from Air Showers in the MHz range at t he Pierre Auger Observatory DTSTART:20140610T141000Z DTEND:20140610T144000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3959@events.icecube.wisc.edu DESCRIPTION:Speakers: Jens Neuser (University of Wuppertal)\, Collaboratio n Pierre Auger (Av. San Martin Norte 306\, 5613 Malargue\, Mendoza\, Argen tina)\n\nThe Auger Engineering Radio Array (AERA) at the Pierre Auger Obse rvatory in Argentinia is constructed in multiple stages starting in 2010. The current stage consists of 124 dual-polarized radio detector stations c overing an area of 6 km^2. One of the main goals is to study the radio emi ssion process for energies beyond 10^{17} eV in the range from 30-80 MHz. Having the unique opportunity for multi-hybrid measurements of air showers alongside the other detectors and also the low-energy extensions at the P ierre Auger Observatory\, AERA is a milestone for further large-scale radi o experiments. Combining the advantages of other detector types\, AERA is investigating the sensitivity to air shower parameters. \n\nThis contribut ion gives an overview of the motivation and science goals of AERA and show s the current status and performance of the detector. First multi-hybrid e vents will be presented as well as the most recent results by the AERA gro up. Polarization measurements which show a strong evidence for a radial po larized component in the electric field vector will be discussed. An outlo ok with future perspectives will be given.\n\nhttps://events.icecube.wisc. edu/event/55/contributions/3959/ URL:https://events.icecube.wisc.edu/event/55/contributions/3959/ END:VEVENT BEGIN:VEVENT SUMMARY:Simulating radio signals from cosmic-ray induced air showers refle cting from a surface DTSTART:20140609T211000Z DTEND:20140609T213000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3960@events.icecube.wisc.edu DESCRIPTION:Speakers: Enrique Zas (Univ. of Santiago de Compostela\, Spain )\, Jaime Alvarez-Muniz (Univ. Santiago de Compostela\, Spain)\, Harm Scho orlemmer (Univ. of Hawaii)\, Washington R. Carvalho Jr. (Univ. of Santiago de Compostela\, Spain)\, Daniel Garcia-Fernandez (Univ. of Santiago de Co mpostela\, Spain)\n\nThe recent detection of radio pulses with the ANITA e xperiment has revealed characteristic signatures of geomagnetic emission a nd has been attributed to coherent radio flashes from air showers that get reflected on the ice cap. In spite of recent progress in simulating and u nderstanding radio pulses from air showers\, no detailed studies are avail able to date to address the impact of the reflection process on the charac teristics of the signal and the extent to which coherence is affected. In this contribution we present a modified version of the ZHAireS code explic itly tailored to calculate radio emission reflected from a surface. We obt ain predictions for the characteristics of the electric field for differen t shower orientations. The results of our simulations \nare understood and validated with a raytracing algorithm and a simple model.\n\nhttps://even ts.icecube.wisc.edu/event/55/contributions/3960/ URL:https://events.icecube.wisc.edu/event/55/contributions/3960/ END:VEVENT BEGIN:VEVENT SUMMARY:Adaptable illumination and calibration of a high-gain antenna for cosmic ray air-shower experiments DTSTART:20140611T190500Z DTEND:20140611T192500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3961@events.icecube.wisc.edu DESCRIPTION:Speakers: Sebastian Mathys (Bergische Universität Wuppertal)\ , Julian Rautenberg (Bergische Universität Wuppertal)\, Karl-Heinz Kamper t (Bergische Univerität Wuppertal)\, Matthias Kleifges (KIT)\, Marc Weber (KIT)\, Radomir Smida (KIT)\, Ralph Engel (KIT)\, Oliver Kroemer (KIT)\, Phillip Papenbreer (Bergische Universität Wuppertal)\, Felix Werner (KIT) \, Lars Petzold (KIT)\n\nAt the Karlsruhe Institute of Technology (KIT) th e microwave detector experiment CROME (Cosmic Ray Observation via Microwav e Emission) has been built up. It was aimed to investigate radio emissions from cosmic ray air showers in L-Band (1.0 to 1.6 GHz) and the extended C -Band (3.4 to 4.2 GHz).\n\nThe final setup used high-gain parabolic reflec tor-type antennas which are illuminated either with cross-polarized dipole s or circular waveguide feeds. Both illumination techniques show an inhomo geneous illumination. The effect can be compensated by using a circular wa veguide feed with movable choke ring after the design of A. Kumar (Reduce cross-polarization in reflector type antennas\, A. Kumar\, Microwaves 1978 ). Due to the expanded near field region \nbeyond 100m of high-gain antenn as\, calibration procedures are challenging. \n\nTo optimize the signal to noise ratio (SNR) we have developed a L-band feed for obtaining a homogen eous illumination of a parabolic reflector-type antenna. We also present a novel method to calibrate such high-gain antennas based on an airborne ca libration transmitter mounted on a GPS-controlled model helicopter. Using this method the design parameters of the feed were verified.\n\nhttps://ev ents.icecube.wisc.edu/event/55/contributions/3961/ URL:https://events.icecube.wisc.edu/event/55/contributions/3961/ END:VEVENT BEGIN:VEVENT SUMMARY:New developments around the Butterfly antenna DTSTART:20140611T153000Z DTEND:20140611T155000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3962@events.icecube.wisc.edu DESCRIPTION:Speakers: Didier CHARRIER (SUBATECH-UMR6457)\n\nThe Butterfly antenna is a compact\, active and dual polarization antenna specifically d eveloped for the radio detection of extensive air showers in the 20-200MHz frequency range. Butterfly antennas are in operations at Nançay for the CODALEMA experiment since october 2008\, and at Auger for the AERA experim ent since may 2013. The overall characteristics of an active antenna are g iven by the antenna itself\, but also by its associated Low Noise Amplifie r (LNA). A new LNA chip named LONAMOS has been designed to enhance the But terfly characteristics. Strong constraints of linearity were imposed in th is design in order to be compliant with the radio-astronomy needs.\n\nBeca use of its characteristics\, the Butterfly antenna has been chosen by many cosmic ray or radio astronomy experiments: 100 antennas for AERA located at the Pierre Auger Observatory (Argentina)\, 67 antennas for CODALEMA (Fr ance)\, 6 antennas for HELYCON (Greece). LNA boards using the LONAMOS chip have also been chosen by other experiments: 55 LNA boards for TREND (Chin a)\, and 4000 LONAMOS chips for NenuFAR located at the Nançay observatory for a radio astronomy array of 1824 antennas.\n\nIn this contribution we will present the Butterfly antenna design keys\, antenna modelization\, ch aracteristics enhancements with the new LONAMOS LNA\, and measurements res ults.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3962/ URL:https://events.icecube.wisc.edu/event/55/contributions/3962/ END:VEVENT BEGIN:VEVENT SUMMARY:Fiber based hydrophones for ultra-high energy neutrino detection DTSTART:20140609T162000Z DTEND:20140609T164000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3963@events.icecube.wisc.edu DESCRIPTION:Speakers: Robert Lahmann (Erlangen Centre for Astroparticle Ph ysics)\, Ernst-Jan Buis (TNO Technical Sciences\, Delft\, The Netherlands) \, Remco Nieuwland (TNO Technical Sciences\, Delft\, The Netherlands)\, Ed Doppenberg (TNO Technical Sciences\, Delft\, The Netherlands)\, Daan van Eijk (TNO Technical Sciences\, Delft\, The Netherlands)\, Peter Toet (TNO Technical Sciences\, Delft\, The Netherlands)\n\nTo survey large volumes o f water for acoustic signals from neutrino interactions\, optical fiber-ba sed hydrophones could potentially have several advantages over conventiona l hydrophones based on piezo ceramics. Optical fibers form a natural way t o create a distributed sensing system in which several sensors are attache d to a single fiber. The detection system in this case will consist of sev eral sensors\, an erbium doped fiber laser and an interferometric interrog ator. Further advantages of this technology are low power consumption and the absence of electromagnetic interference with other read-out electronic s. Maybe even more important\, fiber optics technology provides a cost-eff ective and straightforward way for the installation of a large number of h ydrophones. This allows to establish a large scale experimental set-up wit h tens or hundreds of km^3 detection volume that is required for the expec ted low event rate of neutrino interactions at energies exceeding 10 PeV. \nIn this talk we will discuss the fiber-based hydrophone technology\, fir st measurements performed with test setups and the feasibility of a potent ial future large scale neutrino detector based on fiber-based hydrophones. \n\nhttps://events.icecube.wisc.edu/event/55/contributions/3963/ URL:https://events.icecube.wisc.edu/event/55/contributions/3963/ END:VEVENT BEGIN:VEVENT SUMMARY:GNO - Greenland Neutrino Observatory DTSTART:20140612T130000Z DTEND:20140612T133000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3964@events.icecube.wisc.edu DESCRIPTION:Speakers: Keith Bechtol (KICP\, University of Chicago)\n\nThe goal of the proposed Greenland Neutrino Observatory (GNO) is to discover a nd study ultra-high energy neutrinos by looking for radio emission from pa rticle cascades induced by these neutrinos in the Greenland ice sheet. GNO will consist of an array of radio antenna stations deployed near Summit S tation in central Greenland\, sitting atop a 3 km deep ice sheet. Prelimin ary analysis of field measurements indicate a radio attenuation length of approximately 1000 m at 300 MHz in the upper 1.5 km of ice. We are current ly investigating the logistics of operating at Summit Station\, assembling a prototype station to be deployed in spring/summer 2015\, and developing simulation tools to optimize the design and configuration of the future a rray of antenna stations.\n\nhttps://events.icecube.wisc.edu/event/55/cont ributions/3964/ URL:https://events.icecube.wisc.edu/event/55/contributions/3964/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio Detection of Horizontal Extensive Air Showers with AERA DTSTART:20140611T140000Z DTEND:20140611T142000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3965@events.icecube.wisc.edu DESCRIPTION:Speakers: Olga Kambeitz (IEKP\, KIT)\, Collaboration Pierre Au ger (Pierre Auger Observatory\, Malargüe\, Argentina)\n\nAERA\, the Auger Engineering Radio Array\, located at the Pierre Auger Observatory in Mala rgüe\, Argentina measures the radio emission of extensive air showers in the 30-80 MHz frequency range. It consists of 124 antenna stations of whic h 24 are log periodic dipole antennas (LPDAs) and 100 are so-called butter fly antennas. Both antenna types measure two electric field components (No rth-South and East-West)\nand are optimized for the detection of air showe rs up to 60° zenith angle. Together with the Auger surface detector\, the fluorescence detector\, as well as the muon detector of AMIGA\, AERA is a ble to measure cosmic rays with energies above 10^17 eV in a hybrid detect ion mode.\nSimulation studies have shown that for the reconstruction of in clined air showers the vertical electric field component becomes important . To investigate and improve the sensitivity of AERA to inclined showers\, prototype stations including tripole antenna stations and whisk-type ante nnas as enhancement of the butterfly antennas have been deployed on the AE RA site in November 2013. To study the emission in lower frequencies aroun d 1 MHz one low-frequency tripole station has\nbeen deployed as well.\nIn this contribution the motivation\, the status\, and first results of the a nalysis of horizontal air showers with AERA including the new prototype st ations will be presented.\n\nhttps://events.icecube.wisc.edu/event/55/cont ributions/3965/ URL:https://events.icecube.wisc.edu/event/55/contributions/3965/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterisation of the radio signal emission from extensive air s howers using the SELFAS code DTSTART:20140610T164000Z DTEND:20140610T170000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3966@events.icecube.wisc.edu DESCRIPTION:Speakers: Benoît REVENU (Subatech)\, Vincent MARIN (Subatech) \, Karim Louédec (LPSC)\n\nThe code SELFAS computes the electric field em itted by the secondary electrons and positrons in air showers initiated by high-energy cosmic rays.\nSELFAS is based on the shower universality. We will focus on the main successes of the code to explain observations in th e range MHz-GHz\, and we will insist on the signal emitted by the sudden d eath of air showers when the front disappear in the ground\, in the contex t of the new EXTASIS experiment.\n\nhttps://events.icecube.wisc.edu/event/ 55/contributions/3966/ URL:https://events.icecube.wisc.edu/event/55/contributions/3966/ END:VEVENT BEGIN:VEVENT SUMMARY:More information about DC DTSTART:20140610T170000Z DTEND:20140610T172000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3967@events.icecube.wisc.edu DESCRIPTION:Pick up at Loews is between 1:15 and 1:30 PM. Guide will meet those who want the group tour at Smithsonian Castle on the Mall side. Thi s tour will end at 5:00 PM. Bus will pick up passengers there and take th em to the boat dock - the Dandy Zero on Prince Street in Alexandria\, VA. The cruise will run from 6:30 PM to 9:30 PM\, and includes dinner. The b us will pick up at the pier around 9:40 PM and return everyone to Loews.\n \nhttps://events.icecube.wisc.edu/event/55/contributions/3967/ URL:https://events.icecube.wisc.edu/event/55/contributions/3967/ END:VEVENT BEGIN:VEVENT SUMMARY:SLAC T-510: Radio emission from particle cascades in the presence of a magnetic field DTSTART:20140609T185000Z DTEND:20140609T191500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3968@events.icecube.wisc.edu DESCRIPTION:Speakers: Katharine Mulrey (University of Delaware)\, Konstant in Belov (University of California\, Los Angeles)\, Andrew Romero-Wolf (JP L)\, Stephanie Wissel (University of California\, Los Angeles)\, Collabora tion SLAC T-510 (University of California\, Los Angeles)\n\nGeomagnetic ra diation from air showers is an attractive technique for detecting ultra-hi gh energy cosmic rays. Macroscopic and microscopic models have been develo ped which qualitatively agree with field observations. A controlled labora tory experiment at the Stanford Linear Accelerator Center (SLAC) was desig ned to test these models. The experiment measures the radio frequency emis sion from cascades of secondary particles in a dense dielectric medium in the presence of a magnetic field. The cascades were induced by a ~4.5 GeV electron beam in a polyethylene target placed in magnetic fields up to +/- 1000 G. The radio emission beam pattern was sampled in horizontal and vert ical polarizations by multiple antennas with a total frequency band of 30- 3000MHz. The emission was found to be in good agreement with model predict ions\, including a Cerenkov-like beam pattern and linear scaling with magn etic field.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3968 / URL:https://events.icecube.wisc.edu/event/55/contributions/3968/ END:VEVENT BEGIN:VEVENT SUMMARY:Detection and Characterisation of Microwave Emission of Extensive Air Showers with the CROME Experiment DTSTART:20140610T154000Z DTEND:20140610T161000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3969@events.icecube.wisc.edu DESCRIPTION:Speakers: Felix Werner (KIT)\n\nMicrowave radiation from high- energy air showers has been observed in the C band (3.4–4.2 GHz) with th e Cosmic-Ray Observation via Microwave Emission (CROME) setup. The obtaine d dataset provides a unique opportunity to study the radio emission of air showers at microwave frequencies. The compatibility of the measured GHz s ignals with different hypotheses for the emission mechanism is discussed. It is shown that the component measured in the forward direction of an air shower is compatible with emission mechanisms known from the MHz frequenc y range\, namely the geomagnetic charge separation and charge excess varia tion. Furthermore\, a limit on a potentially isotropic\, unpolarized compo nent\, as expected from molecular bremsstrahlung\, is derived.\n\nhttps:// events.icecube.wisc.edu/event/55/contributions/3969/ URL:https://events.icecube.wisc.edu/event/55/contributions/3969/ END:VEVENT BEGIN:VEVENT SUMMARY:Interferometric Techniques for Radio Impulses from Ultra-high Ener gy Particle Showers DTSTART:20140612T145000Z DTEND:20140612T153000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3970@events.icecube.wisc.edu DESCRIPTION:Speakers: Andrew Romero-Wolf (Jet Propulsion Laboratory)\n\nIn terferometric techniques are widely applied for a variety of radio detecto rs ranging from cosmology (redshifted 21 cm line and cosmic microwave back ground)\, radio astronomy (astrometry\, imaging\, and transient detection) \, and lightning. We present an interferometric technique for the reconstr uction of ultra-wide band impulsive signals from ultra-high energy particl es. This highly sensitive method was developed for the search for ultra-hi gh energy neutrinos with the ANITA experiment but is fully generalizable t o any antenna array detecting radio impulsive events from ultra-high energ y particles. Applications of the interferometric method include event reco nstruction\, thermal noise and anthropogenic background rejection\, and so lar imaging for calibrations. We illustrate this technique with applicatio ns from the analysis of the ANITA-I and ANITA-II data in the 200-1200 MHz band. The ANITA collaboration has been developing a real-time interferomet ric trigger for the detection of ultra-high energy neutrinos and cosmic ra ys. I will discuss some of the key trades required in the application of i nterferometry to a real-time high data rate system. The interferometric tr igger is expected to fly in the ANITA-3 balloon experiment in the 2014-201 5 season.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/3970/ URL:https://events.icecube.wisc.edu/event/55/contributions/3970/ END:VEVENT BEGIN:VEVENT SUMMARY:Introducing TAXI: A Transportable Array for eXtremely large area I nstrumentation studies DTSTART:20140611T161000Z DTEND:20140611T163000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3971@events.icecube.wisc.edu DESCRIPTION:Speakers: Timo Karg (DESY)\, Andreas Haungs (KIT)\, Matthias K leifges (KIT)\, Rolf Nahnhauer (DESY)\n\nA challenge that is common to man y experiments in high-energy astroparticle physics is the need for sparse instrumentation in areas of 100 km2 and above\, often in remote and harsh environments. All these arrays have similar requirements for read-out and communication\, power generation and distribution\, and synchronization. W ithin the TAXI project we are developing a transportable\, modular four-st ation test-array that allows us to study different approaches to solve the aforementioned problems in the laboratory and in the field. Well-defined interfaces will provide easy interchange of the components to be tested an d easy transport and setup will allow in-situ testing at different sites. Every station consists of three well-understood 1 m2 scintillation detecto rs with nanosecond time resolution\, which provide an air shower trigger. An analog sensor\, currently a radio antenna for air shower detection in t he 100 MHz band\, is connected for testing and calibration purposes. We in troduce the TAXI project and report the status and performance of the firs t TAXI station deployed at the Zeuthen site of DESY.\n\nhttps://events.ice cube.wisc.edu/event/55/contributions/3971/ URL:https://events.icecube.wisc.edu/event/55/contributions/3971/ END:VEVENT BEGIN:VEVENT SUMMARY:Welcome DTSTART:20140609T130000Z DTEND:20140609T131000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3972@events.icecube.wisc.edu DESCRIPTION:Speakers: David Seckel (University of Delaware)\, Kara Hoffman (o=umd\,ou=Institutions\,dc=icecube\,dc=wisc\,dc=edu)\n\nhttps://events.i cecube.wisc.edu/event/55/contributions/3972/ URL:https://events.icecube.wisc.edu/event/55/contributions/3972/ END:VEVENT BEGIN:VEVENT SUMMARY:On the feasibility of RADAR detection of high-energy cosmic neutri nos in ice DTSTART:20140611T211500Z DTEND:20140611T213500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3973@events.icecube.wisc.edu DESCRIPTION:Speakers: Krijn de Vries (VUB)\, Hanson Kael (ULB)\, Thomas Me ures (VUB)\, Aongus O'Murchadha (ULB)\n\nWe discuss the radar detection te chnique for the detection of high-energy neutrino-induced particle cascade s in ice. A high-energy neutrino interacting in ice will induce a particle cascade. When propagating through the ice\, this cascade will ionize the medium producing a plasma. The different properties of this ionization pla sma\, such as its size and lifetime\, will be discussed to determine an en ergy threshold for the over-dense scattering of the ionization plasma. Thi s energy threshold is found to be at a few PeV. To determine the feasibili ty of the radar detection technique\, we modeled the radar return power fo r a radio wave scattered off of the ionization plasma for a bi-static rada r configuration. It follows that the radar detection technique\, if succes sful\, will be able to cover the currently existing energy gap between sev eral PeV where IceCube runs out of events and a few EeV where the Askaryan radio detectors start to become sensitive.\n\nhttps://events.icecube.wisc .edu/event/55/contributions/3973/ URL:https://events.icecube.wisc.edu/event/55/contributions/3973/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurements with the absolute calibrated L-band radio antenna of CROME for extensive air showers DTSTART:20140611T184500Z DTEND:20140611T190500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3974@events.icecube.wisc.edu DESCRIPTION:Speakers: Philipp Papenbreer (Bergische Universität Wuppertal )\n\nThe Cosmic-Ray Observation via Microwave Emission (CROME) experiment is designed to study GHz radio emissions from extensive air showers. Multi ple radio antennas measure externally triggered by the KASCADE-Grande air- shower array. The experiment is designed to detect a potentially isotropic \, unpolarized component as expected by molecular bremsstrahlung emission in the low-energy electron plasma indicated by a collider experiment.\nThi s contribution shows the measurements using the L-band (1-2 GHz)\nantenna of CROME. An absolute calibration of the receiver system was\nperformed su ccessfully and could be used for a specific signal search.\nIn addition\, the measurement results were compared to expected field\nstrengths of mole cular bremsstrahlung and simulations of other emission\nmechanisms.\n\nhtt ps://events.icecube.wisc.edu/event/55/contributions/3974/ URL:https://events.icecube.wisc.edu/event/55/contributions/3974/ END:VEVENT BEGIN:VEVENT SUMMARY:A Station For The Detection Of Ultra High Energy Cosmic Ray Induce d Extensive Air Showers At The Telescope Array Radar (TARA) DTSTART:20140611T213500Z DTEND:20140611T215500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3975@events.icecube.wisc.edu DESCRIPTION:Speakers: Samridha Kunwar (The University of Kansas)\n\nThe de tection of high – energy cosmic rays is currently limited by the rarity of the most interesting rays striking Earth. We describe the development o f an observatory based on a remote sensing technique known as bi-static ra dar\, that aims to achieve remote coverage over large portions of the Eart h's surface. The radar project's receiver and transmitter stations have al ready been functional for several months\, in conjunction with North Ameri ca's largest cosmic ray observatory (The Telescope Array) in radio quiet w estern Utah\, giving insight into the detect-ability of air shower radar e choes. This has given impetus for further upgrades\, including additional autonomously powered remote receiver stations. We describe the current sta tus of the Telescope Array RAdar (TARA) project and the development of the se remote stations.\n\nhttps://events.icecube.wisc.edu/event/55/contributi ons/3975/ URL:https://events.icecube.wisc.edu/event/55/contributions/3975/ END:VEVENT BEGIN:VEVENT SUMMARY:The AMY experiment to investigate the GHz emission from air shower plasmas. DTSTART:20140611T180000Z DTEND:20140611T182500Z DTSTAMP:20260912T115100Z UID:indico-contribution-3976@events.icecube.wisc.edu DESCRIPTION:Speakers: Valerio Verzi (Istituto Nazionale Fisica Nucleare)\, Claudio Di Giulio (INFN Tor Vergata)\n\nThe Air Microwave Yield (AMY) exp eriment investigate the molecular bremsstrahlung radiation emitted in the GHz regime from an electron beam induced air-shower . \nThe measurements have been performed with 510 MeV electron beam in a wide frequency range b etween 1 and 20 GHz.
\nWe present the apparatus and the results of the t ests performed at the Beam Test Facility (BTF) of Frascati INFN National L aboratories.\n\nhttps://events.icecube.wisc.edu/event/55/contributions/397 6/ URL:https://events.icecube.wisc.edu/event/55/contributions/3976/ END:VEVENT BEGIN:VEVENT SUMMARY:Digital radio detection of cosmic rays: achievements\, status and perspectives DTSTART:20140610T123000Z DTEND:20140610T131000Z DTSTAMP:20260912T115100Z UID:indico-contribution-3977@events.icecube.wisc.edu DESCRIPTION:Speakers: Tim Huege (Karlsruhe Institute of Technology)\n\nOve r the past decade\, radio detection of cosmic rays has matured from\nsmall -scale prototype experiments to installations spanning several\nkm^2 with more than a hundred antennas. The physics of the radio\nsignal is well und erstood and simulations and measurements are in good\nagreement. We have l earned how to extract important cosmic ray\nparameters such as the geometr y of the air shower and the energy of\nthe primary particle from the radio signal\, and have developed very\npromising approaches to also determine the mass of the primary\nparticles. At the same time\, limitations\, both technical and intrinsic\nto the radio emission physics\, have become incre asingly clear. I will\nreview the progress made in the past decade\, discu ss where the field\nstands and provide a personal view on the limitations of the technique\nand further potential for future development.\n\nhttps:/ /events.icecube.wisc.edu/event/55/contributions/3977/ URL:https://events.icecube.wisc.edu/event/55/contributions/3977/ END:VEVENT END:VCALENDAR