TOMOGRAPHY OF THE
                    <i>FERMI</i>
                    -LAT
                    <i>γ</i>
                    -RAY DIFFUSE EXTRAGALACTIC SIGNAL VIA CROSS CORRELATIONS WITH GALAXY CATALOGS

Xia, Jun-Qing; Cuoco, A.; Branchini, E.; Viel, Matteo

doi:10.1088/0067-0049/217/1/15

Cited by 65 publications

(141 citation statements)

References 88 publications

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“…Bottom: Cross-correlation angular power spectrum between the Fermi data, above 1 GeV, and the 2MASS galaxies, compared with the measurements by Ref. [52]. Model parameters as well as line types are the same as the top panel.…”

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

“…We base this approach on the measurements of Ref. [52], which analyzed the IGRB data and found that they were spatially correlated with galaxy distributions. Compared to the commonly adopted spectral analysis, the tomographic method allows us to efficiently extract a dominant IGRB component in certain redshift ranges following galaxy catalogs, as originally proposed for dark matter detection [53][54][55].…”

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

“…Compared to the commonly adopted spectral analysis, the tomographic method allows us to efficiently extract a dominant IGRB component in certain redshift ranges following galaxy catalogs, as originally proposed for dark matter detection [53][54][55]. This provides stringent constraints on astrophysical sources [52] and dark matter [56].…”

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

“…where δI γ ¼ I γ − hI γ i, δΣ g ¼ Σ g − hΣ g i, P l ðcos θÞ is the Legendre polynomial, and W l is the beam window function (i.e., the Legendre transform of the point spread function of the Fermi LAT [52]). The angular cross-power spectrum C γg l is computed as (e.g., Ref.…”

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

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Tomographic Constraints on High-Energy Neutrinos of Hadronuclear Origin

2015

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Mounting evidence suggests that the TeV-PeV neutrino flux detected by the IceCube telescope has mainly an extragalactic origin. If such neutrinos are primarily produced by a single class of astrophysical sources via hadronuclear (pp) interactions, a similar flux of gamma-ray photons is expected. For the first time, we employ tomographic constraints to pinpoint the origin of the IceCube neutrino events by analyzing recent measurements of the cross correlation between the distribution of GeV gamma rays, detected by the Fermi satellite, and several galaxy catalogs in different redshift ranges. We find that the corresponding bounds on the neutrino luminosity density are up to 1 order of magnitude tighter than those obtained by using only the spectrum of the gamma-ray background, especially for sources with mild redshift evolution. In particular, our method excludes any hadronuclear source with a spectrum softer than E −2.1 as a main component of the neutrino background, if its evolution is slower than ð1 þ zÞ 3 . Starburst galaxies, if able to accelerate and confine cosmic rays efficiently, satisfy both spectral and tomographic constraints. Introduction.-The discovery of the PeV neutrinos by IceCube [1,2] has launched the era of high-energy neutrino astronomy. The current data set is compatible with a flux in excess with respect to the atmospheric background, with an isotropic allocation of events on the celestial sphere and flavor equipartition [1][2][3][4][5][6]. Because of the current low statistics, the origin of the high-energy IceCube events is not yet known, but an extragalactic and mostly diffuse origin appears to be favored [7,8].High-energy neutrino production from cosmic accelerators has been the subject of a cascade of theoretical studies, especially after the IceCube results were announced [7,8]. Many papers discuss the neutrino emission from one specific source class by adopting a modeldependent approach, for active galactic nuclei (AGNs) [9][10][11][12][13][14][15][16][17][18], star-forming galaxies [19][20][21][22][23][24][25][26][27][28], gamma-ray bursts [29][30][31][32][33][34][35][36], galaxy clusters [37][38][39][40], and dark matter decays [41][42][43][44][45].Alternatively, a more generic approach focuses on the phenomenological aspects of the potential sources. For example, assuming photomeson production (pγ) of neutrinos, Ref.[46] obtained constraints on the source size and magnetic field strength needed to match the IceCube flux. Reference [47] hypothesized that the TeV-PeV neutrinos were generated via hadronuclear interactions (pp) and concluded that the cosmic ray spectrum of the dominant neutrino sources should be harder than E −2.2 . This is because the associated gamma-ray spectrum will extend down to GeV energies, where the flux of the isotropic gamma-ray background (IGRB) measured with the Fermi Large Area Telescope (LAT) [48] cannot be overshot. The connection with sources of ultrahigh-energy cosmic rays has also been considered [49][50][51].

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Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

Section: Tomographic Constraints On High-energy Neutrinos Of Hadronucmentioning

confidence: 99%

See 2 more Smart Citations

Tomographic Constraints on High-Energy Neutrinos of Hadronuclear Origin

2015

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“…Among them is to take cross correlations of gamma-ray data with local galaxy catalogs [14,15] and matter distribution through lensing data [16,17]. Although recent measurements of the cross correlations [18][19][20][21] are consistent with the hypothesis of no dark matter signal, they yield tight constraints thereof (e.g., [22]). …”

Section: Introductionmentioning

confidence: 99%

Modelling the flux distribution function of the extragalactic gamma-ray background from dark matter annihilation

Feyereisen

Ando

Lee

2015

J. Cosmol. Astropart. Phys.

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Abstract. The one-point function (i.e., the isotropic flux distribution) is a complementary method to (anisotropic) two-point correlations in searches for a gamma-ray dark matter annihilation signature. Using analytical models of structure formation and dark matter halo properties, we compute the gamma-ray flux distribution due to annihilations in extragalactic dark matter halos, as it would be observed by the Fermi Large Area Telescope. Combining the central limit theorem and Monte Carlo sampling, we show that the flux distribution takes the form of a narrow Gaussian of 'diffuse' light, with an 'unresolved point source' power-law tail as a result of bright halos. We argue that this background due to dark matter constitutes an irreducible and significant background component for point-source annihilation searches with galaxy clusters and dwarf spheroidal galaxies, modifying the predicted signal-to-noise ratio. A study of astrophysical backgrounds to this signal reveals that the shape of the total gamma-ray flux distribution is very sensitive to the contribution of a dark matter component, allowing us to forecast promising one-point upper limits on the annihilation cross section. We show that by using the flux distribution at only one energy bin, one can probe the canonical cross section required for explaining the relic density, for dark matter of masses around tens of GeV.

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Diagnostics of Kappa Distributions from Optically Thin Solar Spectra

Dudík

Dzifčáková

2021

Kappa Distributions

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TOMOGRAPHY OF THE FERMI -LAT γ -RAY DIFFUSE EXTRAGALACTIC SIGNAL VIA CROSS CORRELATIONS WITH GALAXY CATALOGS

Cited by 65 publications

References 88 publications

Tomographic Constraints on High-Energy Neutrinos of Hadronuclear Origin

Tomographic Constraints on High-Energy Neutrinos of Hadronuclear Origin

Modelling the flux distribution function of the extragalactic gamma-ray background from dark matter annihilation

Diagnostics of Kappa Distributions from Optically Thin Solar Spectra

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