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Resolved and unresolved Galactic gamma-ray sources
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The Galactic gamma-ray flux can be described as the sum of two components: the first is due to the emission from an ensemble of discrete sources, and the second is formed by the photons produced by cosmic rays propagating in interstellar space and interacting with gas or radiation fields. The source component is partially resolved as the contributions from individual sources, but a fraction is unresolved and appears as a diffuse flux. Both the unresolved source flux and the interstellar emission flux encode information of great significance for high energy astrophysics, and therefore the separation of these two contributions is very important. In this work we use the distributions in celestial coordinates of the objects contained in the catalogs obtained by the Extensive Air Showers telescopes HAWC and LHAASO to estimate the total luminosity of the Galactic gamma--ray sources and the contribution of unresolved sources to the diffuse gamma--ray flux. This analysis suggests that while the flux from unresolved sources is measurable and important, the dominant contribution to the diffuse flux over most of the celestial sphere is interstellar emission.
Forward citations
Cited by 4 Pith papers
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Summing the catalogued spectra of Galactic gamma-ray sources yields a smooth total spectrum, with a break around 30 TeV, built from individual sources of very different shapes.
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The cosmic-ray sea explains the Galactic $\gamma$-ray and $\nu$ diffuse emissions from GeV to PeV
LHAASO's diffuse gamma-ray data from 1 TeV to 1 PeV are consistent with cosmic-ray sea models that use CALET, DAMPE, and KASCADE spectra, so no extra emission component is required.
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