KASCADE-Grande Limits on the Isotropic Diffuse Gamma-Ray Flux between 100 TeV and 1 EeV

Apel, W. D.; Arteaga‐Velázquez, J. C.; Bekk, K.; Bertaina, M.; Blümer, J.; Bozdog, H.; Brâncuş, I.M.; Cantoni, E.; Чиавасса, А.; Cossavella, F.; Daumiller, K.; Souza, V. de; Pierro, F. Di; Döll, P.; Engel, R.; Zhu, Feng; Fuhrmann, D.; Gherghel-Lascu, A.; Gils, H.J.; Glasstetter, R.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Huege, T.; Kampert, K.H.; Kang, D.; Klages, H. O.; Link, K.; Łuczak, P.; Mathes, H.J.; Mayer, H.J.; Milke, J.; Mitrica, B.; Morello, C.; Oehlschläger, J.; Ostapchenko, S.; Pierog, T.; Rebel, H.; Roth, M.; Schieler, H.; Schoo, S.; Schröder, Frank G.; Sima, O.; Toma, G.; Trinchero, G.; Ulrich, H.; Weindl, A.; Wochele, J.; Zabierowski, J.

doi:10.3847/1538-4357/aa8bb7

Cited by 71 publications

(51 citation statements)

References 33 publications

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“…Observations Energy [GeV] Detected CL upper limits Gamma (γ) Fermi-LAT [20] 10 −2 -10 3 CASA-MIA [26] 10 5 -10 7 90% KASCADE [25] 10 5 -10 7 90% KASCADE-Grande [25] 10 7 -10 8 90% PAO [30,31] 10 9 -10 10 95% TA [34] 10 9 -10 11 95% Proton (p) PAO [37] 10 9 -10 11 84% Anti-proton (p) PAO [37] 10 9 -10 11 84% AMS-02 [21] 10 −1 -10 2 Positron (e + ) AMS-02 [22] 10 −1 -10 3 Neutrino (ν)…”

Section: Crsmentioning

confidence: 99%

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Probing heavy dark matter decays with multi-messenger astrophysical data

Ishiwata

Macías

Ando

et al. 2020

J. Cosmol. Astropart. Phys.

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We set conservative constraints on decaying dark matter particles with masses spanning a very wide range (10 4 − 10 16 GeV). For this we use multimessenger observations of cosmic-ray (CR) protons/antiprotons, electrons/positrons, neutrinos/antineutrinos and gamma rays. Focusing on decays into thebb channel, we simulate the spectra of dark matter yields by using the Dokshitzer-Gribov-Lipatov-Altarelli-Parisi equations and the Pythia package. We then propagate the CRs of dark matter origin till Earth by using the stateof-the-art numerical frameworks CRPropa, GALPROP and HelMod for the solution of the CR transport equation in the extragalactic, Galactic region and the heliosphere, respectively. Conservative limits are obtained by requiring that the predicted dark matter spectra at Earth be less than the observed CR spectra. Overall, we exclude dark matter lifetimes of 10 28 s or shorter for all the masses investigated in this work. The most stringent constraints reach 10 30 s for very heavy dark matter particles with masses in the range 10 11 -10 14 GeV.

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Section: Crsmentioning

confidence: 99%

“…6. Upper bounds from the observations are given by CASA-MIA [26], KASCADE, KASCADE-Grande [25], PAO [30,31] and TA [34]. Fig.…”

Section: Cosmic Ray Fluxesmentioning

confidence: 99%

Probing heavy dark matter decays with multi-messenger astrophysical data

Ishiwata

Macías

Ando

et al. 2020

J. Cosmol. Astropart. Phys.

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“…Ground based gamma ray detectors [7][8][9][10] have also obtained measurements of the diffuse γ ray flux in the TeV energy range for some regions near the Galactic equator. At higher energy (E 20 TeV) there are at present only upper limits for the diffuse flux [11][12][13], however new detectors (such as IceTop and LHAASO) have the sensitivity to extend the observations to the PeV energy range. These measurements of the diffuse Galactic gamma ray flux at very high energy can be very important in the study of a possible space dependence of the CR spectra.…”

Section: Introductionmentioning

confidence: 99%

Diffuse Galactic gamma-ray flux at very high energy

Lipari

Vernetto

2018

Phys. Rev. D

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The observation of the diffuse Galactic gamma ray flux is the most powerful tool to study cosmic rays in different regions of the Galaxy, because the energy and angular distributions of the photons encode information about the density and spectral shape of relativistic particles in the entire MilkyWay. An open problem of fundamental importance is whether cosmic rays in distant regions of the Milky Way have the same spectral shape observed at the Earth or not. If the spectral shape of protons and nuclei is equal in all the Galaxy, the dominant, hadronic component of the diffuse gamma ray flux must have an angular distribution that, after correcting for absorption effects, is energy independent. To study experimentally the validity of this factorization of the energy and angular dependence of the diffuse flux it is necessary to compare observations in a very broad energy range. The extension of the observations to energies Eγ 0.1-10 PeV is of great interest, because it allows the study of the cosmic ray spectra around the feature known as the "knee". The absorption probability for photons in this energy range is not negligible, and distorts the energy and angular distributions of the diffuse flux, therefore a precise calculation of the absorption effects is necessary for the interpretation of the data. In this work we present predictions of the diffuse gamma ray flux at very high energy, constructed under different hypothesis for the space dependence of the cosmic ray energy spectra, and discuss the potential of the observations for present and future detectors.PACS numbers: 98.35Gi,95.85Pw,95.85Ry * Electronic address: paolo.lipari@roma1.infn.it † Electronic address: vernetto@to.infn.it

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“…The arrival directions of these neutrinos are compatible with an isotropic distribution even in the 10 − 100 TeV range, suggesting that a large part of these diffuse neutrinos come from extragalactic sources. Non-observation of diffuse Galactic γ-rays from the Galactic plane and other extended regions independently suggest that the Galactic contribution (e.g., by Fermi bubbles or local supernova remnants) is unlikely to be dominant (Ahlers & Murase 2014; cxy52@psu.edu Apel et al 2017;Abeysekara et al 2017a,b). However, despite extensive efforts, the physical nature of the sources of the diffuse neutrinos still remains in dispute.…”

Section: Introductionmentioning

confidence: 99%

Cumulative Neutrino and Gamma-Ray Backgrounds from Halo and Galaxy Mergers

Yuan

Mészáros

Murase

et al. 2018

ApJ

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The merger of dark matter halos and the gaseous structures embedded in them, such as proto-galaxies, galaxies, and groups and clusters of galaxies, results in strong shocks that are capable of accelerating cosmic rays (CRs) to ∼ > 10 PeV. These shocks will produce high-energy neutrinos and γ-rays through inelastic pp collisions. In this work, we study the contributions of these halo mergers to the diffuse neutrino flux and to the non-blazar portion of the extragalactic γ-ray background. We formulate the redshift dependence of the shock velocity, galactic radius, halo gas content and galactic/intergalactic magnetic fields over the dark matter halo distribution up to a redshift z = 10. We find that high-redshift mergers contribute a significant amount of the cosmic-ray luminosity density, and the resulting neutrino spectra could explain a large part of the observed diffuse neutrino flux above 0.1 PeV up to ∼ PeV. We also show that our model can somewhat alleviate tensions with the extragalactic γ-ray background. First, since a larger fraction of the CR luminosity density comes from high redshifts, the accompanying γ-rays are more strongly suppressed through γγ annihilations with the cosmic microwave background (CMB) and the extragalactic background light (EBL). Second, mildly radiative-cooled shocks may lead to a harder CR spectrum with spectral indices of 1.5 ∼ < s ∼ < 2.0. Our study suggests that halo mergers, a fraction of which may also induce starbursts in the merged galaxies, can be promising neutrino emitters without violating the existing Fermi γ-ray constraints on the non-blazar component of the extragalactic γ-ray background.

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KASCADE-Grande Limits on the Isotropic Diffuse Gamma-Ray Flux between 100 TeV and 1 EeV

Cited by 71 publications

References 33 publications

Probing heavy dark matter decays with multi-messenger astrophysical data

Probing heavy dark matter decays with multi-messenger astrophysical data

Diffuse Galactic gamma-ray flux at very high energy

Cumulative Neutrino and Gamma-Ray Backgrounds from Halo and Galaxy Mergers

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