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Mr Richard Dallier (SUBATECH, Nantes / Radio Observatory of Nançay)07/06/2016, 09:20Invited talkSince 2003, the Nançay Radio Observatory hosts the CODALEMA experiment, dedicated to radio detection of cosmic ray induced extensive air showers. Several instrumental upgrades have been made up to the current setup. CODALEMA is now composed of: - 57 self-triggering radio detection stations working in the 20-250 MHz band and spread over $1~km^2$; - a 13 scintillator array acting as a...Go to contribution page
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Dr Laura Rossetto (Radboud University Nijmegen)07/06/2016, 09:50
The LOw Frequency ARay (LOFAR) is a multipurpose radio antenna array aimed to detect radio signals in the frequency range 10-240 MHz, covering a large surface in Northern Europe with a higher density in Northern Netherlands. The high number density of radio antennas at the LOFAR core in Northern Netherlands allows to detect radio signals emitted by cosmic ray induced air showers, and to...
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Tim Huege (KIT)07/06/2016, 10:10
Radio detection of cosmic-ray air showers requires time synchronization of detectors on a nanosecond level, especially for advanced reconstruction algorithms based on the wavefront curvature and for interferometric analysis approaches. At the Auger Engineering Radio Array, the distributed, autonomous detector stations are time-synchronized via the Global Positioning System which, however, does...
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Clancy James (University of Erlangen-Nuernberg)07/06/2016, 11:00Invited talkThe lunar technique is a method for maximising the collection area for ultra-high-energy (UHE) cosmic ray and neutrino searches. The method uses either ground-based radio telescopes or lunar orbiters to search for Askaryan emission from particles cascading near the lunar surface. While experiments using the technique have made important advances in the detection of nanosecond-scale pulses,...Go to contribution page
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Justin Bray (University of Manchester)07/06/2016, 11:30
The use of the Moon as a detector volume for ultra-high-energy neutrinos and cosmic rays, by searching for the Askaryan radio pulse produced when they interact in the lunar regolith, has been attempted by a range of projects over the past two decades. In this presentation, I will discuss some of the signal-processing considerations relevant to an experiment of this type, with reference to...
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Dr Tobias Winchen (Vrije Universiteit Brussel)07/06/2016, 11:50
The low flux of the ultra-high energy cosmic rays (UHECR) at the highest
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energeis provides a challenge to answer the long standing question about their
origin and nature. A significant increase in the number of detected UHECR is
expected to be achieved by employing Earth's moon as detector, and search for
short radio pulses that are emitted when a particle interacts in the lunar
rock.... -
Sander ter Veen (ASTRON)07/06/2016, 12:10
One of the main ways to use radio to detect Ultra High Energy Neutrinos and Cosmic Rays is the Lunar Askaryan technique, that uses the Moon as a target and searches for nanosecond pulses with large radio telescopes. To use low frequency aperture arrays, such as LOFAR and the SKA, pose new challenges and possibilities in detection techniques of short radio pulses and an accurate measurement of...
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Dr Cosmin Deaconu (UChicago/KICP)07/06/2016, 14:00
The ANtarctic Impulse Transient Antenna (ANITA) collaboration deploys
balloon-borne interferometric antenna payloads that fly at 37 km above Antarctica. The primary goal is detection of Askaryan emission from cosmogenic neutrinos interacting in the ice sheet. In addition, ANITA has proven sensitive to ultra-high-energy cosmic rays.This talk will provide an update on ongoing analyses of...
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Antonio Bonardi (IMAPP - Radboud University Nijmegen)07/06/2016, 14:30
Cosmic rays entering the Earth's atmosphere will produce Extensive Air Showers, which emit a radio signal in the 10-200 MHz frequency region through Geo-synchrotron and Askaryan emission.
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In the last years the Radio detection technique for observing Cosmic rays made huge developments. It has been recently proven that, by using the Radio footprint at the ground-level, the primary particle... -
Julian Rautenberg (Bergische Universität Wuppertal)07/06/2016, 14:50
The Auger Engineering Radio Array (AERA) at the Pierre Auger Observatory with its 153 antenna stations distributed over 17 km2 is the largest experiment to measure the radio emission of extensive air showers.
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The radio emission is known to be influenced by strong atmospheric E-fields such as those in thunderstorm conditions. Based on the measurement of the atmospheric E-field on... -
Gia Trinh (KVI - CART, University of Groningen)07/06/2016, 15:10poster
When a high-energy cosmic-ray particle enters the upper layer of the atmosphere, it generates many secondary high-energy particles and forms a cosmic-ray-induced air shower. In the leading plasma of this shower electric currents are induced that emit electromagnetic radiation. These radio waves can be detected with LOw-Frequency ARray (LOFAR) radio telescope. Events have been collected under...
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Roman Hiller (KIT)07/06/2016, 15:12
The Tunka-Radio extension is a radio detector for air showers in Siberia.
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It currently consists of 44 antennas, distributed over 3 square kilometer, and co-located with Tunka-133, a non-imaging air-Cherenkov detector for air showers.
From 2012 to 2014 on, Tunka-Rex operated exclusively together with its host experiment, Tunka-133, which provided a trigger,
data acquisition and an... -
Krijn de Vries (VUB/IIHE)07/06/2016, 15:14
We discuss the radio emission from different parts of the cascade development for a cosmic-ray induced air shower hitting an ice surface. The in-air emission, in-ice emission, as well as the transition radiation are included in to the calculation. The induced signal should be detectable by the currently operating Askaryan radio detectors searching for the GZK neutrino flux. Where on one side...
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Murat Ali Guler (Middle East Technical University (TR))07/06/2016, 15:16
Nowadays there is compelling evidence for the existence of dark matter in the Universe. A general consensus has been expressed on the need for a directional sensitive detector to confirm, with a complementary approach, the candidates found in “conventional” searches and to finally extend their sensitivity beyond the limit of neutrino-induced background. We propose here the use of a detector...
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Katharine Mulrey (Vrije Universiteit Brussel)07/06/2016, 15:18
LORA (LOFAR Radboud Air shower array) is a particle detector build around the LOFAR core to complement radio detection of cosmic rays. The LORA instrument has been critical in determining the arrival direction, energy, and core location of cosmic rays detected with LOFAR. LORA detects particles from a cosmic ray induced extensive air shower and triggers the LOFAR antennas to read out relevant...
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Mr Danny Sardjan (KVI-CART), Mr Freddie Hendriks (KVI-CART)07/06/2016, 15:20poster
The initial and yet fundamental process in a typical cloud-to-ground lightning strike includes the
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propagation of a very faint and charged channel which is called stepped leader. The exact
mechanism for the step leaders is not understood. The reason for this is that the temporal and/or
spatial resolution of the devices exploited for observing this phenomenon has not been sufficient.
The... -
Rick Timmer (KVI), Sybrand Zeinstra (KVI)07/06/2016, 15:22poster
We present a bottom-up and a top-down model that can produce high-energy neutrinos.
Gamma rays bursts (GRBs) are flashes of gamma rays which are associated with extremely high energetic explosions in distant galaxies. The relativistic fireball is the most popular model to explain the GRBs. Within the fireball model ultra-high energetic cosmic rays can be produced. It is also likely that...
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Lucas van Sloten (KVI)07/06/2016, 15:24poster
Extensive air showers are an interesting phenomena because they can provide information about, among many other things, the electric fields present in the atmosphere, an understanding of which is necessary to understand the concept of lightning.
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To be able to deduce the electric fields from the radio footprint we have developed a macroscopic code that uses a parametrized shower profile. We... -
Eli Waxman07/06/2016, 16:00Invited talkIcecube's discovery of an extra-terrestrial high energy neutrino flux marks the beginning of a new era in neutrino astronomy. I will discuss the what we have learned from this discovery, what the main open questions are, and the way forward towards answering these open questions.Go to contribution page
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Christian Glaser (RWTH Aachen)07/06/2016, 16:30
The Auger Engineering Radio Array (AERA) is an extension of the Pierre Auger Cosmic-Ray Observatory. It is used to detect radio emission from extensive air showers with energies beyond 10$^{17}$ eV in the 30 - 80 MHz frequency band. After three phases of deployment, AERA now consists of more than 150 autonomous radio stations with different spacings, covering an area of about 17 km². It is...
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Katharine Mulrey (Vrije Universiteit Brussel)07/06/2016, 16:50
Cosmic ray induced particle cascades radiate in radio frequencies in the Earth's atmosphere. Geomagnetic and Askaryan emission provide an effective way to detect ultra-high energy cosmic rays. The SLAC T-510 experiment was the first to measure magnetically induced radiation from particle cascades in a controlled laboratory setting. An electron beam incident upon a dense dielectric target...
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Anne Zilles (KIT)07/06/2016, 17:10
The SLAC T-510 experiment was designed to compare controlled laboratory measurements of radio emission of particle showers
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to that predicted using particle-level simulations, which are relied upon in ultra-high-energy cosmic-ray air
shower detection.
Established formalisms for the simulation of radio emission physics, the “end-point” formalism and the “ZHS”
formalism, lead to results... -
Frank Schröder (Karlsruhe Institute of Technology (KIT))08/06/2016, 09:00Invited talkCurrent radio arrays like AERA or Tunka-Rex have demonstrated that areas of several km² can be instrumented for reasonable costs with antenna spacings of the order of 200 m. This finally fulfills the promise that radio detection of air showers can be relatively cheap – at least when radio antennas extend existing arrays. Recent results indicate that for the reconstruction of the energy of the...Go to contribution page
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Frank Schröder (Karlsruhe Institute of Technology (KIT))08/06/2016, 09:30
Tunka-Rex, the Tunka Radio extension, meanwhile consists of 44 SALLA antennas at the TAIGA facility (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) in Siberia, and soon will be extended to a total of 63 antennas, most of them distributed on an area of one square kilometer. In the first years of operation, Tunka-Rex was solely triggered by the co-located air-Cherenkov...
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Florian Briechle (RWTH Aachen University)08/06/2016, 09:50
With the Auger Engineering Radio Array (AERA) located at the Pierre
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Auger Observatory, radio emission of extensive air showers is observed.
To exploit the physics potential of AERA, electric-field amplitude measurements with the radio detector stations need to be well-calibrated on an absolute level. A convenient tool for far-field calibration campaigns is a flying drone. Here we make use of... -
Christian Glaser (RWTH Aachen University)08/06/2016, 10:10
A simulation study of the energy released by extensive air showers in the form of MHz radiation is performed using the CoREAS simulation code. We develop an efficient method to extract this radiation energy from air-shower simulations. We determine the longitudinal profile of the radiation energy release and compare it to the longitudinal profile of the energy deposit by the electromagnetic...
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Robert Lahmann (Friedrich-Alexander-Univ. Erlangen (DE))08/06/2016, 11:00Invited talkThe acoustic neutrino detection technique is a promising approach for future large-scale detectors with the aim of measuring the small expected flux of cosmogenic neutrinos at energies in the EeV-range and above. The technique is based on the thermo-acoustic model, which implies that the energy deposition by a particle cascade - resulting from a neutrino interaction in a medium with suitable...Go to contribution page
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Francesco simeone (Universita e INFN, Roma I (IT))08/06/2016, 11:20Invited talk
In recent years the astro-particle community is involved in the realization of experimental apparatuses for the detection of high energy neutrinos originated in cosmic sources or produced in the interaction of Cosmic Rays with the Cosmic Microwave Background.
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For neutrino energies in the TeV-PeV range, kilometre square optical Cherenkov detector, that has been so far positively exploited by... -
Francesco Simeone, Salvatore Viola (INFN)08/06/2016, 11:45
Acoustic neutrino detectors in water may complement the Cherenkov arrays now under construction (KM3NeT and Baikal) extending the sensitivity of such apparatuses to the Ultra high energy regime.
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In such view the KM3NeT-Italia project has developed acoustic sensors and read-out electronics sensitive to micro-Pascal scale acoustic pulses in the range 5-70 kHz. Read-out and data transmission... -
Francesco Simeone, Salvatore Viola (INFN)08/06/2016, 12:05
In the framework of the KM3NeT-Italia activities, 8 towers, each equipped with 84 large area PMTs for neutrino Cherenkov detection and 29 hydrophones, will be installed. Hydrophones are fully embedded in the electronics and data transport system of the Cherenkov array and are time-synchronised. A data acquisition system (DAQ) on shore has been developed to receive the acoustic stream from sea...
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Dirk Heinen (RWTH Aachen University)08/06/2016, 12:25Contributed talk
In the planned high-energy extension of the IceCube Neutrino Observatory in the deep ice at the geographical South Pole the spacing of detector modules will be increased with respect to IceCube. Because of these larger distances the quality of the optical geometry calibration is expected to deteriorate. To counter this an independent acoustic geometry calibration system based on trilateration...
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Stijn Buitink (Vrije Universiteit Brussel (VUB))09/06/2016, 09:00Invited talkIn the dense core of LOFAR individual air showers are detected by hundreds of dipole antennas simultaneously. We reconstruct Xmax by using a hybrid technique that combines a two-dimensional fit of the radio profile to CoREAS simulations and a one-dimensional fit of the particle density distribution. For high-quality detections, the statistical uncertainty on Xmax is <20 g/cm$^2$. We present...Go to contribution page
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Dmitriy Kostunin (KIT)09/06/2016, 09:30
The Tunka Radio Extension (Tunka-Rex) is a radio detector at TAIGA facility located in Siberia nearby the southern tip of Lake Baikal. Tunka-Rex measures air-showers created by high-energy cosmic rays, in particular the lateral distribution of the radio pulses produced during the development of the air-shower. The depth of the air-shower maximum, which statistically depends on the mass of the...
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Florian Gaté (SUBATECH)09/06/2016, 09:50
One of the current methods to estimate the mass of a cosmic ray is the measurement of the atmospheric depth of the shower maximum ($X_\text{max}$). This depth is strongly correlated to the mass of the primary because it depends on the interaction cross section of the primary with the constituents of the atmosphere. The radio-electric field emitted by the secondary particles of an atmospheric...
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20. The influence of the atmospheric refractive index on radio measurements of extensive air showersArthur Corstanje (Radboud University Nijmegen)09/06/2016, 10:10
Measurements of radio emission from extensive air showers, together with air shower simulations, have allowed to infer the height of maximum emission ($X_{\rm max}$) for individual air showers to a precision of 18 g/cm$^2$, important for composition studies.
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In this procedure, one of the major systematic uncertainties arises from variations of the refractive index in the atmosphere. The... -
Prof. Nikolay Budnev (Irkutsk State University)09/06/2016, 11:00Invited talkThe features, advantage and difficulties of acoustic detection of high energy neutrinos in Fresh water are discussed. The status and perspectives of the feasibility study to detect high energy cosmic neutrinos acoustically in Lake Baikal is presented. A concept of acoustic array as a part of Baikal Gigaton Volume Neutrino Telescope NT1000 based on results of simulation and background...Go to contribution page
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Dominik Kießling (Universität Erlangen-Nürnberg)09/06/2016, 11:30
The research infrastructure KM3NeT will comprise a multi cubic kilometer neutrino telescope that is currently being constructed in the Mediterranean Sea. The telescope will be composed of several detection units anchored at the sea bed, which are kept taut vertically by a buoy. Each detection unit has a length of about 700 hundred meters. Modules with optical and acoustical sensors are mounted...
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Dr Ernst-Jan Buis (TNO)09/06/2016, 11:50
The scientific prospects of detecting neutrinos with an energy close or even higher
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than the GKZ cut-off energy has been discussed extensively in literature. It is clear
that due to their expected low flux, the detection of these ultra-high energy neutrinos
($E_\nu > 10^{18}$ eV ) requires an telescope larger than 100 km$^3$. Acoustic detection [1, 2]
may provide a way to observe these... -
Dirk Heinen (RWTH Aachen University)09/06/2016, 12:10Contributed talk
Within the Enceladus Explorer Initiative of the DLR Space Administration navigation technologies for future space mission are in development. Those technologies are the basis for the search of extraterrestrial life on the Saturn moon Enceladus. An autonomous melting probe, the EnEx-Probe, aims to extract a liquid sample from the ocean below the icy crust.
A first EnEx-Probe was developed...
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Dr Mike van der Schaar (Universitat Politècnica de Catalunya)09/06/2016, 14:00Invited talk
The ANTARES project, in addition to optical detectors, includes an array of 36
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hydrophones that was installed with the aim of acoustic neutrino detection. The
acoustic data stream has been active since 2008 and is managed under AMADEUS.
Coincidentally, ANTARES is installed in the Pelagos marine sanctuary, home to
many marine mammals species, both whales and dolphins, all of which... -
Dr Anna Nelles (University of California Irvine)09/06/2016, 14:30Invited talkThe ARIANNA experiment is currently taking data in its pilot-phase on the Ross ice-shelf. Nine fully autonomous stations measure radio signals in the frequency range from 100 MHz to 1 GHz. The seven station HRA was completed in December 2014, and augmented by two special purpose stations with unique configurations. In its full extent ARIANNA is targeted at detecting interactions of cosmogenic...Go to contribution page
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Prof. Kael Hanson (University of Wisconsin - Madison)09/06/2016, 15:00Invited talkAbstract TBDGo to contribution page
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Keiichi Mase (Chiba University)09/06/2016, 15:30
Askaryan Radio Array (ARA) is being built at the South Pole aiming
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for observing high energy cosmogenic neutrinos above 10 PeV.
The ARA detector identifies the radio emissions from the excess
charge in a particle shower induced by a neutrino interaction. Such
a radio emission was first predicted by Askaryan in 1962 and
experimentally confirmed by Saltzberg et al. using the SLAC... -
Mr Ming-Yuan Lu (University of Wisconsin-Madison)09/06/2016, 16:20
The Askaryan Radio Array (ARA) is a neutrino telescope array under phased deployment near the South Pole. The array aims at discovering and determining the ultra-high energy neutrino flux via detection of the Askaryan signal from neutrino-induced showers. This novel detection channel makes ARA the most cost-effective neutrino observatory in probing the neutrino flux from ~ 100PeV – 10EeV....
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Carl Gilbert Pfendner (Ohio State University (USA))09/06/2016, 16:40
The Askaryan Radio Array (ARA) is a radio frequency observatory under construction at the South Pole that is searching for ultrahigh energy neutrinos via the Askaryan effect. Thermal fluctuations currently dominate the trigger-level background for the observatory and anthropogenic sources also introduce a significant source of noise. By taking advantage of the observatory's regular geometry...
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Jaime Alvarez-Muniz (Universidad de Santiago de Compostela)09/06/2016, 17:00Contributed talkWe explore transition radiation at MHz-GHz frequencies as a possible way to detect ultrahigh-energy (UHE) particles. We have developed a general method to calculate transition radiation that extends the well-known Zas-Halzen-Stanev (ZHS) algorithm. We have applied it to the characterization of the frequency and angular properties of the electric field from high-energy showers crossing the...Go to contribution page
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Krijn de Vries (VUB/IIHE)09/06/2016, 17:20
A detailed model for the radar reflection of in-ice particle cascades is presented. This allows us to determine the effective area and sensitivity for a typical bi-static radar set-up. It follows that the radar technique is a promising method to probe the currently existing energy gap between several PeV where IceCube runs low in statistics and a few EeV where the Askaryan radio detectors...
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Prof. Stephanie Wissel (Cal Poly)10/06/2016, 09:00Invited talkIn-ice radio arrays are optimized for detecting the highest energy, cosmogenic neutrinos, expected to be produced though cosmic ray interactions with background photons. However, there are two expected populations of high energy neutrinos: the astrophysical flux observed by IceCube (\~1 PeV) and the cosmogenic flux (\~10$^{18}$ eV or 1000 PeV). Typical radio arrays employ a noise-riding...Go to contribution page
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Olivier Martineau (CNRS)10/06/2016, 09:30
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Carl Gilbert Pfendner (Ohio State University (USA))10/06/2016, 09:50
A flux of ultrahigh energy neutrinos is expected both directly from sources and from interactions between ultrahigh energy cosmic rays and the cosmic microwave background. Using the cost-effective radio Cherenkov technique to search for these neutrinos, the ExaVolt Antenna (EVA) is a mission concept that aims to build on the capabilities of earlier radio-based balloon-borne neutrino detectors...
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Dr Arjen van Vliet (Radboud University Nijmegen)10/06/2016, 10:10Contributed talk
With our newly-developed code for ultra-high-energy cosmic ray (UHECR) propagation, CRPropa, the flux of neutrinos due to interactions of UHECRs with extragalactic background light can be predicted. These cosmogenic neutrinos cover a wide energy range, from below PeV energies up till 100 EeV. The recent measurements in the PeV range and limits at higher energies from IceCube are starting to...
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Tim Huege (KIT)10/06/2016, 11:00As of 2023, the low-frequency part of SKA-1 will go online in Australia. It will constitute the largest and most powerful low-frequency radio-astronomical observatory to date, and will facilitate a rich science programme in astronomy and astrophysics. With modest engineering changes, SKA-1 low will also be able to measure cosmic rays via the radio emission from extensive air showers. The...Go to contribution page
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Anne Zilles (KIT)10/06/2016, 11:30
As LOFAR has shown, using a dense array of radio antennas for detecting extensive air showers initiated by cosmic rays in the Earth’s atmosphere makes it possible to
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measure the depth of shower maximum for individual showers with a statistical uncertainty less than $20\,\mbox{g/cm}^2$. This allows detailed studies of the mass composition in the energy region around $10^{17}\mbox{eV}$ where... -
Olga Kambeitz10/06/2016, 11:50
The Auger Engineering Radio Array (AERA), located at the Pierre Auger Observatory in
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Argentina, measures the radio emission of extensive air showers in the 30-80 MHz
frequency range. AERA consists of more than 150 antenna stations distributed over 17 km^2.
Together with the Auger surface detector, the fluorescence detector and the muon detector
(AMIGA), AERA is able to measure cosmic rays... -
10/06/2016, 12:10
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María Saldaña Coscollar (UPV), Miguel Ardid (UPV)
Acoustic detection is a promising technique for the detection of Ultra High Energy (UHE) neutrinos. It is based on the detection of the short bipolar pressure pulse with very directive pattern (pancake) generated after the neutrino interaction with a nucleus of the water. The acoustic sensors could be implemented in the optical-based deep-sea neutrino telescope under construction (KM3NeT...
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