Limits on the flux of ultrahigh-energy neutrinos from radio astronomical observations

Beresnyak, Andrey; Дагкесаманский, Р. Д.; Железных, И. М.; Kovalenko, A. V.; Oreshko, V. V.

doi:10.1134/1.1862359

Cited by 71 publications

(86 citation statements)

References 15 publications

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“…The simulation for the Kalyazin experiment is somewhat simpler, needing only to model a singly-triggered data channel. See Gorham et al [9] and Beresnyak et al [20] for details of these experiments.…”

Section: Modelling Neutrino Detection Experimentsmentioning

confidence: 99%

“…Since the regolith is comparatively transparent at radio frequencies, coherent Cherenkov emission from sufficiently high-energy particle interactions (specifically, from UHE cosmic ray and neutrino interactions) in the regolith should be detectable by Earth-based radio-telescopes. First attempted by Hankins, Ekers & O'Sullivan [19] using the Parkes radio telescope, subsequent experiments at Goldstone (GLUE) [9] and Kalyazin [20] have placed limits on an isotropic flux of UHE neutrinos. Observations continue at both Westerbork (WSRT) [21] and the Australia Telescope Compact Array (ATCA; our project), and the technique has been the subject of several theoretical and Monte Carlo studies [22,23,24,25] together with our own recent work [26].…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Modelling Neutrino Detection Experimentsmentioning

confidence: 99%

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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“…For a wide bandwidth, the effect is to stretch the pulse out in time and to reduce its peak amplitude, particularly at low frequencies. Early experiments looked in multiple frequency bands for coincident pulses, separated by an offset corresponding to the dispersive delay [8,10]. Others, operating at high frequencies with relatively narrow bandwidths, simply neglected the minor dispersive effects [9,14].…”

Section: Ionospheric Dispersionmentioning

confidence: 99%

“…The first lunar particle detection experiment was performed in 1995 with the Parkes radio telescope [8]; subsequent experiments have been carried out with the Goldstone Deep Space Communications Complex (GDSCC) [9,GLUE], the Kalyazin radio telescope [10], the Australia Telescope Compact Array (ATCA) [11,LUNASKA], the Lovell telescope [12,La Luna], the Westerbork Synthesis Radio Telescope (WSRT) [13,NuMoon] and the Expanded Very Large Array (EVLA) [14,RESUN]. A key feature of these experiments is that they make use of existing radio telescopes, whereas other experiments searching for UHE cosmic rays or neutrinos require the development of expensive dedicated instruments.…”

Section: Introductionmentioning

confidence: 99%

A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

Bray

Ekers

Roberts

et al. 2015

Astroparticle Physics

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We describe an experiment using the Parkes radio telescope in the 1.2-1.5 GHz frequency range as part of the LUNASKA project, to search for nanosecond-scale pulses from particle cascades in the Moon, which may be triggered by ultra-highenergy astroparticles. Through the combination of a highly sensitive multi-beam radio receiver, a purpose-built backend and sophisticated signal-processing techniques, we achieve sensitivity to radio pulses with a threshold electric field strength of 0.0053 µV/m/MHz, lower than previous experiments by a factor of three. We observe no pulses in excess of this threshold in observations with an effective duration of 127 hours. The techniques we employ, including compensating for the phase, dispersion and spectrum of the expected pulse, are relevant for future lunar radio experiments.

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“…The second was the Goldstone Lunar Ultra-high energy neutrino Experiment (GLUE) [12] that used two large telescopes of the JPL/NASA Deep Space Network in Goldstone (CA). A third experiment of this kind took place at Kalyazin Radio Astronomical Observatory, using again a single 64 m radio telescope [13]. None of these experiments however, resulted in any detection of signals from UHE particles.…”

Section: Introductionmentioning

confidence: 99%

Prospects for the Giant Metrewave Radio Telescope to observe radio waves from ultra high energy particles interacting with the Moon

Panda

Mohanty

Janardhan

et al. 2007

J. Cosmol. Astropart. Phys.

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Ultra high energy (UHE) particles of cosmic origin impact the lunar regolith and produce radio signals through Askaryan effect, signals that can be detected by Earth based radio telescopes. We calculate the expected sensitivity for observation of such events at the Giant Metrewave Radio Telescope (GMRT), both for UHE cosmic rays (CR) and UHE neutrino interactions. We find that for 30 days of observation time a significant number of detectable events is expected above 10 20 eV for UHECR or neutrino fluxes close to the current limits. Null detection over a period of 30 days will lower the experimental bounds by a magnitude competitive to both present and future experiments at the very highest energies.

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Limits on the flux of ultrahigh-energy neutrinos from radio astronomical observations

Cited by 71 publications

References 15 publications

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

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

A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

Prospects for the Giant Metrewave Radio Telescope to observe radio waves from ultra high energy particles interacting with the Moon

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