SIMBAD references

2014ApJ...782..109D - Astrophys. J., 782, 109 (2014/February-3)

Diffuse pionic gamma-ray emission from large-scale structures in the Fermi era.

DOBARDZIC A. and PRODANOVIC T.

Abstract (from CDS):

For more than a decade now, the complete origin of the diffuse gamma-ray emission background (EGRB) has been unknown. Major components like unresolved star-forming galaxies (making ≲ 50% of the EGRB) and blazars ( ≲ 23%), have failed to explain the entire background observed by Fermi. Another, though subdominant, contribution is expected to come from the process of large-scale structure formation. The growth of structures is accompanied by accretion and merger shocks, which would, with at least some magnetic field present, give rise to a population of structure-formation cosmic rays (SFCRs). Though expected, this cosmic-ray population is still hypothetical and only very weak limits have been placed to their contribution to the EGRB. The most promising insight into SFCRs was expected to come from Fermi-LAT observations of clusters of galaxies, however, only upper limits and no detection have been placed. Here, we build a model of gamma-ray emission from large-scale accretion shocks implementing a source evolution calibrated with the Fermi-LAT cluster observation limits. Though our limits to the SFCR gamma-ray emission are weak (above the observed EGRB) in some cases, in others, some of our models can provide a good fit to the observed EGRB. More importantly, we show that these large-scale shocks could still give an important contribution to the EGRB, especially at high energies. Future detections of cluster gamma-ray emission would help place tighter constraints on our models and give us a better insight into large-scale shocks forming around them.

Abstract Copyright:

Journal keyword(s): cosmic rays - diffuse radiation - gamma rays: diffuse background - gamma rays: galaxies: clusters - large-scale structure of universe

Errata: erratum vol. 787, art. 95 (2014)

Simbad objects: 2

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2019.12.15-21:48:38

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