Comparative study of electromagnetic shower track lengths in water and implications for Čerenkov radio emission

Álvarez-Muñiz, J.; Marqués, Enrique; Vázquez, R. A.; Zas, E.

doi:10.1103/physrevd.68.043001

Cited by 21 publications

(15 citation statements)

References 31 publications

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“…Radio-wavelength detection of electromagnetic showers in ice relies on two experimentally established phenomena -long attenuation lengths exceeding 1 km, and coherence extending up to 1 GHz for Cherenkov emission. Discussions of the Askaryan effect [1] upon which the radiowave detection technique is founded, its experimental verification in a testbeam environment [16,17], calculations of the expected radio-frequency signal from a purely electromagnetic shower [18][19][20][21][22][23], as well as hadronic showers [24], and modifications due to the LPM effect [25,26] can be found in the literature.…”

Section: A Signal Strengthmentioning

confidence: 99%

Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

et al. 2012

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The RICE experiment seeks observation of ultra-high energy ("UHE"; E ν > 10 17 eV) neutrinos interacting in Antarctic ice, by measurement of the radio frequency (RF) Cherenkov radiation resulting from the collision of a neutrino with an ice molecule. RICE was initiated in 1999 as a first-generation prototype for an eventual, large-scale in-ice UHE neutrino detector. Herein, we present updated limits on the diffuse UHE neutrino flux, based on twelve years of data taken between 1999 and 2010. We find no convincing neutrino candidates, resulting in 95% confidencelevel model-dependent limits on the flux E 2 ν dφ/dE ν < 0.5 × 10 −6 GeV/(cm 2 s − sr) in the energy range 10 17 < E ν < 10 20 eV, or approximately a two-fold improvement over our previously published results. Recently, the focus of RICE science has shifted to studies of radio frequency ice properties as the RICE experimental hardware has been absorbed into a new experimental initiative (the Askaryan Radio Array, or 'ARA') at South Pole. ARA seeks to improve on the RICE sensitivity by approximately two orders of magnitude by 2017 and thereby establish the cosmogenic neutrino flux. As detailed herein, RICE studies of Antarctic ice demonstrate that both birefringence and internal layer RF scattering result in no significant loss of ARA neutrino sensitivity, and, for the first time, verify in situ the decrease in attenuation length with depth into the Antarctic ice sheet.

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Section: A Signal Strengthmentioning

confidence: 99%

Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

et al. 2012

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“…Ref. [19]). If the interaction medium is transparent to radio waves, the radiation can readily escape from the medium and be detected remotely.…”

Section: The Lunar Cherenkov Techniquementioning

confidence: 99%

“…Observations continue at both WSRT [25] and with our own project using the ATCA and using the Parkes radio telescope (to be reported elsewhere). The technique has been the subject of several theoretical and Monte Carlo studies [19,[26][27][28][29] together with our own recent work [22,30,31].…”

Section: The Lunar Cherenkov Techniquementioning

confidence: 99%

LUNASKA experiments using the Australia Telescope Compact Array to search for ultrahigh energy neutrinos and develop technology for the lunar Cherenkov technique

et al. 2010

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We describe the design, performance, sensitivity and results of our recent experiments using the Australia Telescope Compact Array (ATCA) for lunar Cherenkov observations with a very wide (600 MHz) bandwidth and nanosecond timing, including a limit on an isotropic neutrino flux. We also make a first estimate of the effects of small-scale surface roughness on the effective experimental aperture, finding that contrary to expectations, such roughness will act to increase the detectability of near-surface events over the neutrino energy-range at which our experiment is most sensitive (though distortions to the time-domain pulse profile may make identification more difficult). The aim of our "Lunar UHE Neutrino Astrophysics using the Square Kilometer Array" (LUNASKA) project is to develop the lunar Cherenkov technique of using terrestrial radio telescope arrays for ultra-high energy (UHE) cosmic ray (CR) and neutrino detection, and in particular to prepare for using the Square Kilometer Array (SKA) and its path-finders such as the Australian SKA Pathfinder (ASKAP) and the Low Frequency Array (LOFAR) for lunar Cherenkov experiments.

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“…ref. [17]). If the interaction medium is transparent to radio waves, the radiation can readily escape from the medium and be detected remotely.…”

Section: Introductionmentioning

confidence: 99%

The sensitivity of the next generation of lunar Cherenkov observations to UHE neutrinos and cosmic rays

James

Protheroe

2009

Astroparticle Physics

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We present simulation results for the detection of ultra-high energy (UHE) cosmic ray (CR) and neutrino interactions in the Moon by radio-telescopes. We simulate the expected radio signal at Earth from such interactions, expanding on previous work to include interactions in the sub-regolith layer for single dish and multiple telescope systems. For previous experiments at Parkes, Goldstone, and Kalyazin we recalculate the sensitivity to an isotropic flux of UHE neutrinos. Our predicted sensitivity for future experiments using the Australia Telescope Compact Array (ATCA) and the Australian SKA Pathfinder (ASKAP) indicate these instruments will be able to detect the more optimistic UHE neutrino flux predictions, while the Square Kilometre Array (SKA) will also be sensitive to all bar one prediction of a diffuse 'cosmogenic', or 'GZK', neutrino flux.Current uncertainties concerning the structure and roughness of the lunar surface prevents an accurate calculation of the sensitivity of the lunar Cherenkov technique for UHE cosmic ray astronomy at high frequencies. However, below 200 MHz we find that the proposed SKA lowfrequency aperture array should be able to detect events above 56 EeV at a rate about 30 times that of the current Pierre Auger Observatory. This would allow directional analysis of UHE cosmic rays, and investigation of correlations with putative cosmic ray source populations, to be conducted with very high statistics.

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Comparative study of electromagnetic shower track lengths in water and implications for Čerenkov radio emission

Cited by 21 publications

References 31 publications

Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

LUNASKA experiments using the Australia Telescope Compact Array to search for ultrahigh energy neutrinos and develop technology for the lunar Cherenkov technique

The sensitivity of the next generation of lunar Cherenkov observations to UHE neutrinos and cosmic rays

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