Spectrum of the Extra-galactic Background Radiation at Low Radio Frequencies

Clark, T. A.; Brown, L. W.; Alexander, J. K.

doi:10.1038/228847a0

Cited by 82 publications

(102 citation statements)

References 9 publications

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“…Fig. 12 shows the results for m X = 2 × 10 14 GeV, with B = 10 −12 G, and again the minimal URB consistent with data [59,77]. These parameters lead to optimistic neutrino fluxes for the maximal normalization consistent with all data.…”

Section: Neutrino Fluxes In Top-down Scenariossupporting

confidence: 51%

Ultrahigh-energy neutrino fluxes and their constraints

et al. 2002

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Applying our recently developed propagation code we review extragalactic neutrino fluxes above 10 14 eV in various scenarios and how they are constrained by current data. We specifically identify scenarios in which the cosmogenic neutrino flux above ≃ 10 18 eV, produced by pion production of ultra high energy cosmic rays outside their sources, is considerably higher than the "WaxmanBahcall bound". This is easy to achieve for sources with hard injection spectra and luminosities that were higher in the past. Such fluxes would significantly increase the chances to detect ultra-high energy neutrinos with experiments currently under construction or in the proposal stage.

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Section: Neutrino Fluxes In Top-down Scenariossupporting

confidence: 51%

Ultrahigh-energy neutrino fluxes and their constraints

et al. 2002

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“…In addition to the CMB photons, we consider in these calculations all other main photon targets in the intergalactic medium. The universal radio background (URB) is considered in this study only for the development of electromagnetic cascades; for this purpose we conservatively use the spectrum given in Clark et al (1970) and the cosmological evolution estimated in Lee (1998). Several authors have already treated the impact of different estimates of the radio background on the output of electromagnetic cascades (see for instance Gelmini et al 2008;Taylor & Aharonian 2009).…”

Section: Modeling the Propagation Of Cosmic Rays And Electromagnetic mentioning

confidence: 99%

Constraints on the origin of ultra-high-energy cosmic rays from cosmogenic neutrinos and photons

Decerprit¹,

Allard

2011

A&A

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We study the production of cosmogenic neutrinos and photons during the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs). For a wide range of models in cosmological evolution of source luminosity, composition and maximum energy we calculate the expected flux of cosmogenic secondaries by normalizing our cosmic ray output to experimental spectra and comparing the diffuse flux of GeV−TeV gamma-rays to the experimental one measured by the Fermi satellite. Most of these models yield significant neutrino fluxes for current experiments like IceCube or Pierre Auger. Furthermore, we discuss the possibilities of signing the presence of UHE proton sources either within or outside the cosmic ray horizon using neutrinos or photons observations even if the cosmic ray composition becomes heavier at the highest energies. We discuss the possible constraints that could be brought on the UHECR origin from the different messengers and energy ranges.

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“…The mean effective electron loss length is calculated following Gabici & Aharonian (2005), using the radio background data of Clark et al (1970). We assume that each electron emits a synchrotron photon spectrum dN γ /dE γ ∝ E −2/3 γ with a sharp cut-off above E c ∼ (2/3) E γ,syn , where E γ,syn is given by Eq.…”

Section: Numerical Codementioning

confidence: 99%

Detectability of ultrahigh energy cosmic-ray signatures in gamma-rays

Kotera

Allard

Lemoine

2011

A&A

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The injection of ultrahigh energy cosmic-rays in the intergalactic medium leads to the production of a GeV-TeV gamma-ray halo centered on the source location, through the production of a high electromagnetic component in the interactions of the primary particles with the radiation backgrounds. This paper examines the prospects for the detectability of such gamma-ray halos. We explore a broad range of astrophysical parameters, including the inhomogeneous distribution of magnetic fields in the large-scale structure, as well as various possible chemical compositions and injection spectra; and we consider the case of a source located outside clusters of galaxies. We demonstrate that the gamma-ray flux associated to synchrotron radiation of ultrahigh energy secondary pairs does not depend strongly on these parameters, and conclude that its magnitude ultimately depends on the energy injected into the primary cosmic-rays. We find that the gamma-ray halo produced by equal luminosity sources (with cosmic ray luminosity and source density chosen to reproduce the measured cosmic-ray spectrum) is far fainter than current or planned instrument sensitivities. Only rare and powerful steady sources, located at distances larger than several hundreds of Mpc and contributing to a fraction 10% of the flux at 10 19 eV might be detectable. We also discuss the gamma-ray halos that are produced by inverse Compton/pair production cascades seeded by ultrahigh energy cosmic-rays. This depends strongly on the configuration of the extragalactic magnetic fields; it is dominated by the synchrotron signal on a degree scale if the filling factor of magnetic fields with B 10 −14 G is smaller than a few percent. Finally, we briefly discuss the case of nearby potential sources such as Centaurus A.

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Spectrum of the Extra-galactic Background Radiation at Low Radio Frequencies

Cited by 82 publications

References 9 publications

Ultrahigh-energy neutrino fluxes and their constraints

Ultrahigh-energy neutrino fluxes and their constraints

Constraints on the origin of ultra-high-energy cosmic rays from cosmogenic neutrinos and photons

Detectability of ultrahigh energy cosmic-ray signatures in gamma-rays

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