Neutrino Astronomy

Ishihara, A.

doi:10.22323/1.236.0013

Cited by 4 publications

(9 citation statements)

References 22 publications

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“…This confirmed a major prediction of Albert Einstein's 1915 General Theory of Relativity and opened up an unprecedented new window to the Universe: gravitational wave astronomy [1] next to neutrino astronomy [2].…”

Section: Editorialsupporting

confidence: 60%

On the History of the Michelson Experiment: A Personal Recollection (Gravitational Waves Detected 100 Years After Einstein's General Relativity)

J¹,

Haubold²

2016

Astrobiol Outreach

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Section: Editorialsupporting

confidence: 60%

On the History of the Michelson Experiment: A Personal Recollection (Gravitational Waves Detected 100 Years After Einstein's General Relativity)

J¹,

Haubold²

2016

Astrobiol Outreach

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“…Also in this case, the energy scale of the proton spectrum has been shifted according to the value δ E obtained. The plot also shows the upper limit on the neutrino flux obtained by IceCube at 90% CL [23]. The data points at low energies correspond to the spectrum of the EGB observed by Fermi-LAT [32].…”

Section: Fit Of the Uhecr Spectrummentioning

confidence: 89%

“…In Ref. [22] the dip model has been rejected at 95% CL by using the upper limit on the neutrino spectrum obtained by the IceCube experiment [23]. In that work the source evolution is assumed to be the one corresponding to the star formation rate times (1 + z) m where z is the redshift and m is a parameter fixed by fitting Telescope Array data.…”

Section: Introductionmentioning

confidence: 99%

Implications of gamma-ray observations on proton models of ultrahigh energy cosmic rays

Supanitsky

2016

Phys. Rev. D

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The origin of ultra high energy cosmic rays (UHECR) is still unknown. However, great progress has been achieved in past years due to the good quality and large statistics in experimental data collected by the current observatories. The data of the Pierre Auger Observatory show that the composition of the UHECRs becomes progressively lighter starting from 10 17 eV up to ∼ 10 18.3 eV and then, beyond that energy, it becomes increasingly heavier. These analyses are subject to important systematic uncertainties due to the use of hadronic interaction models that extrapolate lower energy accelerator data to the highest energies. Although proton models of UHECRs are disfavored by these results, they cannot be completely ruled out. It is well known that the energy spectra of gamma rays and neutrinos, produced during propagation of these very energetic particles through the intergalactic medium, are a useful tool to constrain the spectrum models. In particular, it has recently been shown that the neutrino upper limits obtained by IceCube challenge the proton models at 95% CL. In this work we study the constraints imposed by the extragalactic gamma-ray background, measured by Fermi-LAT, on proton models of UHECRs. In particular, we make use of the extragalactic gamma-ray background flux, integrated from 50 GeV to 2 TeV, that originates in point sources, which has recently been obtained by the Fermi-LAT collaboration, in combination with the neutrino upper limits, to constrain the emission of UHECRs at high redshits (z > 1), in the context of the proton models.

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“…2 6, m = 1 and z max = 5 normalized on TA spectrum [41]. Also, the Fermi IGRB measurements are shown for galactic foreground model B, as well as secondary ν-spectrum along with IceCube neutrino 'differential flux' upper limit [18]. The Fermi LAT constraint of Eq.…”

Section: A Standard Proton Modelsmentioning

confidence: 98%

Cascade photons as test of protons in UHECR

Berezinsky

Gazizov

Kalashev

2016

Astroparticle Physics

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An isotropic component of high energy $\gamma$-ray spectrum measured by Fermi LAT constrains the proton component of UHECR. The strongest restriction comes from the highest, $(580-820)$ GeV, energy bin. One more constraint on the proton component is provided by the IceCube upper bound on ultrahigh energy cosmogenic neutrino flux. We study the influence of these restrictions on the source properties, such as evolution and distribution of sources, their energy spectrum and admixture of nuclei. We also study the sensitivity of restrictions to various Fermi LAT galactic foreground models (model B being less restrictive), to the choice of extragalactic background light model and to overall normalization of the energy spectrum. We claim that the $\gamma$-ray-cascade constraints are stronger than the neutrino ones, and that however many proton models are viable. The basic parameters of such models are relatively large $\gamma_g$ and not very large $z_{\max}$. The allowance for H$e^4$ admixture also relaxes the restrictions. However we foresee that future CTA measurements of $\gamma$-ray spectrum at $E_\gamma \simeq (600 - 800)$ GeV, as well as resolving of more individual $\gamma$-ray sources, may rule out the proton-dominated cosmic ray models.Comment: Version accepted for publication in Astroparticle Physics. Most recent neutrino flux limits by IceCube were included to the tables. 14 pages, 13 figure

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Neutrino Astronomy

Cited by 4 publications

References 22 publications

On the History of the Michelson Experiment: A Personal Recollection (Gravitational Waves Detected 100 Years After Einstein's General Relativity)

On the History of the Michelson Experiment: A Personal Recollection (Gravitational Waves Detected 100 Years After Einstein's General Relativity)

Implications of gamma-ray observations on proton models of ultrahigh energy cosmic rays

Cascade photons as test of protons in UHECR

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