Diffuse Emission of Galactic High-energy Neutrinos from a Global Fit of Cosmic Rays

Schwefer, Georg; Mertsch, Philipp; Wiebusch, C. H.

doi:10.3847/1538-4357/acc1e2

Cited by 19 publications

(18 citation statements)

References 135 publications

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“…We defer further investigations on these questions to future studies. In this domain we expect important synergies between CTA and neutrino observatories [98][99][100][101]. Synergies with HAWC, LHAASO and Fermi-LAT will also be crucial as these instruments have a much better handle on the CR background modelling.…”

Section: Interstellar Emissionmentioning

confidence: 99%

Survey of the Galactic Plane with the Cherenkov Telescope Array

Remy¹,

Tibaldo²,

Acero³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Observations with the current generation of very-high-energy gamma-ray telescopes have revealed an astonishing variety of particle accelerators in the Milky Way, such as supernova remnants, pulsar wind nebulae, and binary systems. The upcoming Cherenkov Telescope Array (CTA) will be the first instrument to enable a survey of the entire Galactic plane in the energy range from a few tens of GeV to 300 TeV with unprecedented sensitivity and improved angular resolution. In this contribution we will revisit the scientific motivations for the survey, proposed as a Key Science Project for CTA. We will highlight recent progress, including improved physically-motivated models for Galactic source populations and interstellar emission, advance on the optimization of the survey strategy, and the development of pipelines to derive source catalogues tested on simulated data. Based on this, we will provide a new forecast on the properties of the sources that CTA will detect and discuss the expected scientific return from the study of gamma-ray source populations.

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Section: Interstellar Emissionmentioning

confidence: 99%

Survey of the Galactic Plane with the Cherenkov Telescope Array

Remy¹,

Tibaldo²,

Acero³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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“…In Figures 3 and 5, the GP flux corresponds to the IceCube measurement using the shower data and the π 0 template (Abbasi et al 2023). Another IceCube analysis using tracks (Fuerst et al 2023) yields a similar flux with π 0 and CRINGE (Schwefer et al 2023) templates. Comparing to the π 0 and CRINGE flux, the GP flux derived from the shower data (Abbasi et al 2023) with the KRA templates (Gaggero et al 2015) is similar above ∼10 TeV but 3-5 times lower around 1 TeV.…”

Section: Appendix D Neutrino Emission From All Sourcesmentioning

confidence: 71%

“…Figure 6. and derived all-flavor neutrino flux from GDE averaged over the full sky (warm colors, unhatched) comparing with models, including the KRA models (Gaggero et al 2015), the CRINGE models (Schwefer et al 2023), and the HNR model (Ahlers & Murase 2014).…”

Section: Appendix D Neutrino Emission From All Sourcesmentioning

confidence: 99%

Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations

Fang,

Murase

2023

ApJL

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High-energy neutrino and γ-ray emission has been observed from the Galactic plane, which may come from individual sources and/or diffuse cosmic rays. We evaluate the contribution of these two components through the multimessenger connection between neutrinos and γ-rays in hadronic interactions. We derive maximum fluxes of neutrino emission from the Galactic plane using γ-ray catalogs, including 4FGL, HGPS, 3HWC, and 1LHAASO, and measurements of the Galactic diffuse emission by Tibet ASγ and LHAASO. We find that the IceCube Galactic neutrino flux is larger than the contribution from all resolved sources when excluding promising leptonic sources such as pulsars, pulsar wind nebulae, and TeV halos. Our result indicates that the Galactic neutrino emission is likely dominated by the diffuse emission by the cosmic-ray sea and unresolved hadronic γ-ray sources. In addition, the IceCube flux is comparable to the sum of the flux of nonpulsar sources and the LHAASO diffuse emission especially above ∼30 TeV. This implies that the LHAASO diffuse emission may dominantly originate from hadronic interactions, either as the truly diffuse emission or unresolved hadronic emitters. Future observations of neutrino telescopes and air-shower γ-ray experiments in the Southern hemisphere are needed to accurately disentangle the source and diffuse emission of the Milky Way.

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“…Particularly, LHAASO measured diffuse emission from the outer Galactic plane for the first time, which can give more comprehensive constraints on the CR distribution in the Galaxy. Based on improved measurements of the local CR spectra and diffuse emission, one can better constrain the CR injection, propagation, and interaction in the Milky Way (Schwefer et al 2023;Marinos et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

Zhang,

Huang,

et al. 2023

ApJ

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Diffuse γ-ray emission between 10 and 1000 TeV from the Galactic plane was recently measured by the Large High Altitude Air Shower Observatory (LHAASO). These observations will help tremendously in constraining the propagation and interaction of cosmic rays in the Milky Way. Additionally, new measurements of cosmic-ray spectra reach a very high precision of up to 100 TeV energies, revealing multiple spectral structures of various species. In this work, based on up-to-date measurements of local cosmic-ray spectra and a simplified propagation setup, we confront a model prediction of diffuse γ-ray emission with measurements of diffuse γ-rays. To better constrain the low-energy part of the model, we analyze the 14.6 yr of Fermi Large Area Telescope (Fermi-LAT) data to extract the Galactic diffuse emission between 1 and 500 GeV from the same sky regions of LHAASO, after subtracting the contribution from known sources and the isotropic diffuse γ-ray background. The joint Fermi-LAT and LHAASO spectra thus cover a very wide energy range from 1 GeV to 1 PeV with small gaps from 0.5 to 10 TeV. Compared with the prediction, we find that clear excesses between several GeV and ∼60 TeV of the diffuse emission exist. Possible reasons to explain the excesses may include unresolved sources or more complicated propagation models. We illustrate that an exponential cutoff power-law component with an index of −2.40 and a cutoff energy of ∼30 TeV is able to account for such excesses.

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Diffuse Emission of Galactic High-energy Neutrinos from a Global Fit of Cosmic Rays

Cited by 19 publications

References 135 publications

Survey of the Galactic Plane with the Cherenkov Telescope Array

Survey of the Galactic Plane with the Cherenkov Telescope Array

Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations

Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements

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