Conveners
Presentations
- Jaime Alvarez-Muniz (Universidad de Santiago de Compostela)
Presentations
- Sijbrand De Jong (Radboud University Nijmegen (NL))
Presentations: Presentations
- Richard Dallier (SUBATECH, Nantes / Radio Observatory of Nanรงay)
Presentations: Presentations
- Kael Hanson (University of Wisconsin - Madison)
Presentations: Presentations
- Jรถrg Hรถrandel (Ru Nijmegen/Nikhef)
Presentations: Presentations
- R. Lahmann (-)
Presentations: Presentations
- Tim Huege (KIT)
Presentations: Presentations
- Antonio Capone (Universita e INFN, Roma I (IT))
Presentations: Presentations
- Stephanie Wissel (Cal Poly)
Presentations: Presentations
- Keiichi Mase (Chiba University)
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- Julian Rautenberg (Bergische Universitรคt Wuppertal)
Presentations: Presentations
- Rolf Nahnhauer (Institut fuer Hochenergiephysik Zeuthen)
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...
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...
The low flux of the ultra-high energy cosmic rays (UHECR) at the highest
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....
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...
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.
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...
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.
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...
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 kmยฒ. It is...
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...
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...
With the Auger Engineering Radio Array (AERA) located at the Pierre
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...
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...
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.
For neutrino energies in the TeV-PeV range, kilometre square optical Cherenkov detector, that has been so far positively exploited by...
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.
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...
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...
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...
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.
In this procedure, one of the major systematic uncertainties arises from variations of the refractive index in the atmosphere. The...
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...
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...
The ANTARES project, in addition to optical detectors, includes an array of 36
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...
Askaryan Radio Array (ARA) is being built at the South Pole aiming
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...
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 โ 10EeV....
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...
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...
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...
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...
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...
