The Antarctic Impulsive Transient Antenna ultra-high energy neutrino detector: Design, performance, and sensitivity for the 2006–2007 balloon flight

Gorham, P. W.; Allison, P.; Barwick, S. W.; Beatty, J. J.; Besson, D.; Binns, W. R.; Chen, C.; Chen, P.; Clem, J.; Connolly, A.; Dowkontt, P. F.; DuVernois, M. A.; Field, R. C.; Goldstein, David J.; Goodhue, A.; Hast, C.; Hébert, Christian; Hoover, S.; Israel, M. H.; Kowalski, J.; Learned, J. G.; Liewer, K. M.; Link, J. T.; Lusczek, Elizabeth R.; Matsuno, S.; Mercurio, B. C.; Miki, C.; Miočinović, P.; Nam, J. W.; Naudet, C. J.; Nichol, R. J.; Palladino, K. J.; Reil, K.; Romero-Wolf, Andrés; Rosen, M.; Ruckman, L.; Saltzberg, D.; Seckel, D.; Varner, G.; Walz, D.; Wang, Y.; Williams, Christopher S.; Wu, Fan

doi:10.1016/j.astropartphys.2009.05.003

Cited by 192 publications

(165 citation statements)

References 48 publications

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“…[38,39,40,41] and neutrinos (right) [52] obtained from the Pierre Auger Observatory. The data are shown together with the current limits from other experiments [53,54,55,56,57,58,59] and some examples of predicted fluxes.…”

Section: Uhe Photon and Neutrino Limitsmentioning

confidence: 99%

Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory

Molina Bueno

2015

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Section: Uhe Photon and Neutrino Limitsmentioning

confidence: 99%

Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory

Molina Bueno

2015

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“…Left: Picture of the ANITA payload. Taken from [1]. Right: voltage as a function of time for the 16 cosmic ray events detected by ANITA.…”

Section: The Experimentsmentioning

confidence: 99%

“…The ANITA experiment [1], originally conceived for the detection of the radio emission coming from neutrino-induced showers, detected 16 pulses emitted by cosmic ray showers. Out of those 16 radio pulses, 14 were reflected on the polar ice cap [2].…”

Section: Introductionmentioning

confidence: 99%

Measurement of the cosmic ray flux with the ANITA experiment

et al. 2017

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Abstract. The ANITA experiment consists on an aerostatic balloon flying over Antarctica and carrying a payload with antennas. Although ANITA was designed to detect the electric field of netrino-induced showers in the ice cap, it has also detected 16 radio pulses coming from extensive air showers, and the ANITA collaboration has used these data to produce the first cosmic ray flux measurement obtained by employing radio as a standalone technique. We review the experimental results and its interpretation. We also focus on the simulations and the method used for obtaining the cosmic ray flux.

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“…Such emission has been measured and characterized at beam-line experiments [4,5,6]. This technique has been exploited by several experiments in Antarctica, including ANITA [7], ARA [8], and ARIANNA [9]. These experiments have thresholds > 50 PeV, however, recent studies have shown improved sensitivity to the PeV energy scale using phased arrays of antennas [10,11], which would complement studies of the few-PeV astrophysical neutrino signal discovered by IceCube [12].…”

Section: Introductionmentioning

confidence: 99%

Site Characterization and Detector Development for the Greenland Neutrino Observatory

Wissel¹,

Avva²,

Bechtol³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The PeV neutrinos discovered by IceCube are of astrophysical origin, and their progenitors could be any of several source classes, including active galactic nuclei, gamma-ray bursts, or pulsars. Such high-energy accelerators would produce neutrinos up to hundreds of PeV, which motivates the development of neutrino telescopes with the sensitivity, energy resolution, and pointing resolution required to distinguish among models of the IceCube neutrinos as well as cosmogenic neutrinos. Radio detection of Askaryan radiation from neutrino showers in ice is well-suited to the detection of the highest energy neutrinos, with degree-scale pointing resolution and the ability to build sparse arrays, but the energy threshold of current experiments is currently set by the temperature of the ice. The uncorrelated thermal noise can be reduced by combining the signals from several antennas in a phased array. We report here on a June 2015 trip to Summit Station In Greenland for testing a phased array of dipoles, as well as the sensitivity of the array and background measurements of the site and discuss prospects for the Greenland Neutrino Observatory (GNO).

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The Antarctic Impulsive Transient Antenna ultra-high energy neutrino detector: Design, performance, and sensitivity for the 2006–2007 balloon flight

Cited by 192 publications

References 48 publications

Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory

Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory

Measurement of the cosmic ray flux with the ANITA experiment

Site Characterization and Detector Development for the Greenland Neutrino Observatory

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