Limits on deeply penetrating particles in the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>&gt;</mml:mo><mml:mn>10</mml:mn><mml:mn /></mml:mrow><mml:mrow><mml:mn>17</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>eV cosmic-ray flux

Baltrusaitis, R. M.; Cassiday, G. L.; Elbert, J. W.; Gerhardy, P. R.; Loh, E. C.; Mizumoto, Y.; Sokolsky, P.; Steck, D.

doi:10.1103/physrevd.31.2192

Cited by 91 publications

(121 citation statements)

References 20 publications

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“…However, experiments to date have not found showers with a deficiency of muons (see, for example, Inoue et al, 1999a), and for the most energetic event detected (3ϫ10 20 eV) the shower profile does not have the characteristics expected if the primary were a photon (Halzen et al, 1995). The Fly's Eye group (Baltrusaitis, Cassiday, et al, 1985) has set an upper limit to the flux of high-energy neutrinos, but this does not seriously challenge the predictions which are orders of magnitude lower. It follows that future detectors should be constructed with the capability of gamma-ray and neutrino detection: a measurement of these fluxes would be of great help in addressing the question of the origin of the UHECRs.…”

Section: E Neutrinos and Gamma Raysmentioning

confidence: 99%

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Observations and implications of the ultrahigh-energy cosmic rays

2000

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The authors define ''ultrahigh-energy cosmic rays'' (UHECRs) as those cosmic rays with energies above 10 18 eV. It had been anticipated that there would be a cutoff in the energy spectrum of primary cosmic rays around 6ϫ10 19 eV induced by the interaction of the particles with the 2.7-K primordial photons. However, recent experimental data have established that particles exist with energies greatly exceeding this. It follows that the sources of such particles are probably nearby, on a cosmological scale. However, although the trajectories of such energetic particles through the galactic and intergalactic magnetic fields may be nearly rectilinear, no astronomical sources have as yet been identified. This is the enigma of the highest-energy cosmic rays. The paper reviews the history of research in this energy regime and critically assesses the observational results on the energy spectrum, arrival directions, and composition of the primary cosmic rays based on observations made by six experiments. The detection methods currently available are described. Special techniques have been developed as particles of 10 20 eV or higher occur at a rate of only about 1 per km 2 per century. Errors in measurement are given particular attention. The authors also review the theoretical predictions for a number of candidate sources of cosmic rays beyond the predicted cutoff. Finally, the four major projects planned to address the question of the origin of UHECRs are briefly described. CONTENTS

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Section: E Neutrinos and Gamma Raysmentioning

confidence: 99%

“…Baltrusaitis, Cassiday, et al (1985) searched for deeply penetrating showers and upward-moving showers above 10 17 eV with the Fly's Eye detector and no unusual events were found in 6ϫ10 6 sec of running time.…”

Section: Deeply Penetrating Primary Particlesmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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“…As a result, roughly 90% of the energy in hadronic showers is EM. The response and efficiency of fluorescence detectors to hadronic and EM showers is therefore expected to be similar [18]. In this work we adopt the total Fly's Eye exposure reported in Ref.…”

Section: Neutrino Exposurementioning

confidence: 99%

Neutrino bounds on astrophysical sources and new physics

et al. 2002

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Ultra-high energy cosmic neutrinos are incisive probes of both astrophysical sources and new TeV-scale physics. Such neutrinos would create extensive air showers deep in the atmosphere. The absence of such showers implies upper limits on incoming neutrino fluxes and cross sections. Combining the exposures of AGASA, the largest existing ground array, with the exposure of the Fly's Eye fluorescence detector integrated over all its operating epochs, we derive 95% CL bounds that substantially improve existing limits. We begin with model-independent bounds on astrophysical fluxes, assuming standard model cross sections, and model-independent bounds on new physics cross sections, assuming a conservative cosmogenic flux. We then derive model-dependent constraints on new components of neutrino flux for several assumed power spectra, and we update bounds on the fundamental Planck scale M D in extra dimension scenarios from black hole production. For large numbers of extra dimensions, we find M D > 2.0 (1.1) TeV for M min BH = M D (5M D ), comparable to or exceeding the most stringent constraints to date.

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“…The region with the solid boundary is obtained by a cosmological evolution parameter n = 3. Boxes show the upper bounds obtained by combining Fly's Eye [13] and Agasa [14] limits on deeply penetrating showers in different energy bins [15]. According to these limits, strong cosmological evolution (n > 3) for the sources of the post-GZK events is already excluded.…”

Section: Propagation Inversionmentioning

confidence: 99%

“…(4)). Boxes show the upper bounds obtained by combining Fly's Eye [13] and Agasa [14] limits on deeply-penetrating showers in different energy bins [15]. The dotted band labelled by Auger represents the expected sensitivity of the Pierre Auger Observatory to ν τ +ν τ , corresponding to one event per year per energy decade [16].…”

Section: Propagation Functionsmentioning

confidence: 99%

Bounds on the cosmogenic neutrino flux

Fodor¹,

Katz²,

Ringwald³

et al. 2003

J. Cosmol. Astropart. Phys.

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Under the assumption that some part of the observed highest energy cosmic rays consists of protons originating from cosmological distances, we derive bounds on the associated flux of neutrinos generated by inelastic processes with the cosmic microwave background photons. We exploit two methods. First, a power-like injection spectrum is assumed. Then, a modelindependent technique, based on the inversion of the observed proton flux, is presented. The inferred lower bound is quite robust. As expected, the upper bound depends on the unknown composition of the highest energy cosmic rays. Our results represent benchmarks for all ultrahigh energy neutrino telescopes.

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Limits on deeply penetrating particles in the>1017eV cosmic-ray flux

Cited by 91 publications

References 20 publications

Observations and implications of the ultrahigh-energy cosmic rays

Observations and implications of the ultrahigh-energy cosmic rays

Neutrino bounds on astrophysical sources and new physics

Bounds on the cosmogenic neutrino flux

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