A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2

Mottram, M.

doi:10.1007/978-3-642-30032-5

Cited by 4 publications

(3 citation statements)

References 41 publications

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“…• Background events often cluster in time, in position, or both, because sources are either static (e.g., high-voltage power lines) or follow a trajectory (e.g., an airplane in flight), and often emit radio signals in bursts. For example, ANITA-2 filtered out 99% of their total events using a cluster analysis [274]. TREND reached a similar performance, at the cost of ∼10% loss in EAS detection efficiency [162].…”

Section: Background Rejectionmentioning

confidence: 97%

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

Álvarez-Muñiz

Batista

Balagopal

et al. 2019

Sci. China Phys. Mech. Astron.

255

279

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The Giant Radio Array for Neutrino Detection (GRAND) 1 is a planned large-scale observatory of ultra-highenergy (UHE) cosmic particles -cosmic rays, gamma rays, and neutrinos with energies exceeding 10 8 GeV. Its ultimate goal is to solve the long-standing mystery of the origin of UHE cosmic rays. It will do so by detecting an unprecedented number of UHECRs and by looking with unmatched sensitivity for the undiscovered UHE neutrinos and gamma rays associated to them. Three key features of GRAND will make this possible: its large exposure at ultra-high energies, sub-degree angular resolution, and sensitivity to the unique signals made by UHE neutrinos.The strategy of GRAND is to detect the radio emission coming from large particle showers that develop in the terrestrial atmosphereextensive air showers -as a result of the interaction of UHE cosmic rays, gamma, rays, and neutrinos. To achieve this, GRAND will be the largest array of radio antennas ever built. The relative affordability of radio antennas makes the scale of construction possible. GRAND will build on years of progress in the field of radio-detection and apply the large body of technological, theoretical, and numerical advances, for the first time, to the radio-detection of air showers initiated by UHE neutrinos.The design of GRAND will be modular, consisting of several independent sub-arrays, each of 10 000 radio antennas deployed over 10 000 km 2 in radio-quiet locations. A staged construction plan ensures that key techniques are progressively validated, while simultaneously achieving important science goals in UHECR physics, radioastronomy, and cosmology early during construction.Already by 2025, using the first sub-array of 10 000 antennas, GRAND could discover the long-sought cosmogenic neutrinos -produced by interactions of ultra-high-energy cosmic-rays with cosmic photon fields -if their flux is as high as presently allowed, by reaching a sensitivity comparable to planned upgraded versions of existing experiments. By the 2030s, in its final configuration of 20 sub-arrays, GRAND will reach an unparalleled sensitivity to cosmogenic neutrino fluxes of 4 • 10 −10 GeV cm −2 s −1 sr −1 within 3 years of operation, which will guarantee their detection even if their flux is tiny. Because of its sub-degree angular resolution, GRAND will also search for point sources of UHE neutrinos, steady and transient, potentially starting UHE neutrino astronomy. Because of its access to ultra-high energies, GRAND will chart fundamental neutrino physics at these energies for the first time.GRAND will also be the largest detector of UHE cosmic rays and gamma rays. It will improve UHECR statistics at the highest energies ten-fold within a few years, and either discover UHE gamma rays or improve their limits ten-fold. Further, it will be a valuable tool in radioastronomy and cosmology, allowing for the discovery and follow-up of large numbers of radio transients -fast radio bursts, giant radio pulses -and for precise studies of the epoch of reionization.Following the disc...

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Section: Background Rejectionmentioning

confidence: 97%

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

Álvarez-Muñiz

Batista

Balagopal

et al. 2019

Sci. China Phys. Mech. Astron.

255

279

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“…Determining the response of the antenna is the most difficult part of the whole calibration. Antennas for higher frequencies of several 100 MHz are usually small enough for accurate measurements of their free-space response in anechoic chambers by the two-antenna method, as has been done for the ANITA horn antennas [298]. Antennas for the frequency band of 30 − 80 MHz are larger, which would require large anechoic chambers.…”

Section: Response Of Antenna Stationsmentioning

confidence: 99%

Radio detection of cosmic-ray air showers and high-energy neutrinos

Schröder

2017

Progress in Particle and Nuclear Physics

175

129

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In the last fifteen years radio detection made it back to the list of promising techniques for extensive air showers, firstly, due to the installation and successful operation of digital radio experiments and, secondly, due to the quantitative understanding of the radio emission from atmospheric particle cascades. The radio technique has an energy threshold of about 100 PeV, which coincides with the energy at which a transition from the highest-energy galactic sources to the even more energetic extragalactic cosmic rays is assumed. Thus, radio detectors are particularly useful to study the highest-energy galactic particles and ultra-high-energy extragalactic particles of all types. Recent measurements by various antenna arrays like LOPES, CODALEMA, AERA, LOFAR, Tunka-Rex, and others have shown that radio measurements can compete in precision with other established techniques, in particular for the arrival direction, the energy, and the position of the shower maximum, which is one of the best estimators for the composition of the primary cosmic rays. The scientific potential of the radio technique seems to be maximum in combination with particle detectors, because this combination of complementary detectors can significantly increase the total accuracy for air-shower measurements. This increase in accuracy is crucial for a better separation of different primary particles, like gamma-ray photons, neutrinos, or different types of nuclei, because showers initiated by these particles differ in average depth of the shower maximum and in the ratio between the amplitude of the radio signal and the number of muons. In addition to air-shower measurements, the radio technique can be used to measure particle cascades in dense media, which is a promising technique for detection of ultra-high-energy neutrinos. Several pioneering experiments like ARA, ARIANNA, and ANITA are currently searching for the radio emission by neutrino-induced particle cascades in ice. In the next years these two sub-fields of radio detection of cascades in air and in dense media will likely merge, because several future projects aim at the simultaneous detection of both, high-energy cosmic-rays and neutrinos. SKA will search for neutrino and cosmic-ray initiated cascades in the lunar regolith and simultaneously provide unprecedented detail for air-shower measurements. Moreover, detectors with huge exposure like GRAND, SWORD or EVA are being considered to study the highest energy cosmic rays and neutrinos. This review provides an introduction to the physics of radio emission by particle cascades, an overview on the various experiments and their instrumental properties, and a summary of methods for reconstructing the most important air-shower properties from radio measurements. Finally, potential applications of the radio technique in high-energy astroparticle physics are discussed.

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“…3 for all six combinations of flavor and interaction channels, an upper limit for the total exposure of the two first ANITA flights for neutrino detection with the TR is plotted in Fig. 4 In the same plot we also display the exposures of other experiments searching for cosmogenic neutrinos: the analysis of ANITA when trying to detect Askaryan radiation from neutrino-induced showers in ice [26], assuming the same live time T a ; approximately nine years of data collected at the Pierre Auger Observatory [7]; and preliminary results of six years of IceCube [4]. For Ice-Cube we used the neutrino effective area from [27] with data taken in several periods of time with various string configurations [4,27].…”

Section: Total Exposurementioning

confidence: 99%

Can transition radiation explain the ANITA event 3985267?

et al. 2017

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We investigate whether transition radiation from a particle shower crossing the interface between Earth and air and induced by an Earth-skimming neutrino can explain the upward event announced recently by the ANITA Collaboration. While the properties of the observed signal can in principle be explained with transition radiation, a conservative upper limit on the experiment's aperture for this kind of signal shows that the flux necessary for a successful explanation is in tension with the current best limits from the Pierre Auger Observatory, the IceCube neutrino detector and the ANITA balloon. We also show that in this scenario, the direction of the incoming neutrino is determined precisely to within a few degrees, combining the polarization properties of the observed events with the Earth opacity to ultra high energy neutrinos.

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A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2

Cited by 4 publications

References 41 publications

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

Radio detection of cosmic-ray air showers and high-energy neutrinos

Can transition radiation explain the ANITA event 3985267?

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